Author name code: moore-ron ADS astronomy entries on 2022-09-14 author:"Moore, Ronald L." OR author:"Moore, Ron" NOT =author:"Moore, R.C." NOT =author:"Moore, R.D." -title:"IceCube" -title:"neutrino" -title:"neutron star" ------------------------------------------------------------------------ Title: Density of GeV muons in air showers measured with IceTop Authors: Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alameddine, J. M.; Alves, A. A.; Amin, N. M.; Andeen, K.; Anderson, T.; Anton, G.; Argüelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K. -H.; Becker Tjus, J.; Beise, J.; Bellenghi, C.; Benda, S.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Brinson, B.; Bron, S.; Brostean-Kaiser, J.; Browne, S.; Burgman, A.; Burley, R. T.; Busse, R. S.; Campana, M. A.; Carnie-Bronca, E. G.; Chen, C.; Chen, Z.; Chirkin, D.; Choi, K.; Clark, B. A.; Clark, K.; Classen, L.; Coleman, A.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J. J.; Delgado López, D.; Dembinski, H.; Deoskar, K.; Desai, A.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Diaz, A.; Díaz-Vélez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M. A.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fedynitch, A.; Feigl, N.; Fiedlschuster, S.; Fienberg, A. T.; Finley, C.; Fischer, L.; Fox, D.; Franckowiak, A.; Friedman, E.; Fritz, A.; Fürst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glüsenkamp, T.; Gonzalez, J. G.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Günther, C.; Gutjahr, P.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Ha Minh, M.; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; Hymon, K.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G. S.; Jeong, M.; Jin, M.; Jones, B. J. P.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Kardum, L.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K.; Kintscher, T.; Kiryluk, J.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lazar, J. P.; Lee, J. W.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q. R.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K. B. M.; Makino, Y.; Mancina, S.; Mariş, I. C.; Martinez-Soler, I.; Maruyama, R.; McCarthy, S.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Mechbal, S.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyên, L. V.; Niederhausen, H.; Nisa, M. U.; Nowicki, S. C.; Obertacke Pollmann, A.; Oehler, M.; Oeyen, B.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D. V.; Park, N.; Parker, G. K.; Paudel, E. N.; Paul, L.; Pérez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Pries, B.; Przybylski, G. T.; Raab, C.; Rack-Helleis, J.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rechav, Z.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E. J.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S. E.; Sandrock, A.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Shimizu, N.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Stezelberger, T.; Stürwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Ter-Antonyan, S.; Thwaites, J.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M. A.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Veitch-Michaelis, J.; Verpoest, S.; Walck, C.; Wang, W.; Watson, T. B.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M. J.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D. R.; Wolf, M.; Wrede, G.; Wulff, J.; Xu, X. W.; Yanez, J. P.; Yildizci, E.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z.; Zhelnin, P.; IceCube Collaboration Bibcode: 2022PhRvD.106c2010A Altcode: 2022arXiv220112635A We present a measurement of the density of GeV muons in near-vertical air showers using three years of data recorded by the IceTop array at the South Pole. Depending on the shower size, the muon densities have been measured at lateral distances between 200 and 1000 m. From these lateral distributions, we derive the muon densities as functions of energy at reference distances of 600 and 800 m for primary energies between 2.5 and 40 PeV and between 9 and 120 PeV, respectively. The muon densities are determined using, as a baseline, the hadronic interaction model Sibyll 2.1 together with various composition models. The measurements are consistent with the predicted muon densities within these baseline interaction and composition models. The measured muon densities have also been compared to simulations using the post-LHC models EPOS-LHC and QGSJet-II.04. The result of this comparison is that the post-LHC models together with any given composition model yield higher muon densities than observed. This is in contrast to the observations above 1 EeV where all model simulations yield for any mass composition lower muon densities than the measured ones. The post-LHC models in general feature higher muon densities so that the agreement with experimental data at the highest energies is improved but the muon densities are not correct in the energy range between 2.5 and about 100 PeV. Title: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra Authors: Panesar, Navdeep K.; Tiwari, Sanjiv K.; Moore, Ronald L.; Sterling, Alphonse C.; De Pontieu, Bart Bibcode: 2022arXiv220900059P Altcode: We present the first IRIS Mg II slit-raster spectra that fully capture the genesis and coronal-jet-generating eruption of a central-disk solar minifilament. The minifilament arose in a negative-magnetic-polarity coronal hole. The Mg II spectroheliograms verify that the minifilament plasma temperature is chromospheric. The Mg II spectra show that the erupting minifilament's plasma has blueshifted upflow in the jet spire's onset and simultaneous redshifted downflow at the location of the compact jet bright point (JBP). From the Mg II spectra together with AIA EUV images and HMI magnetograms, we find: (i) the minifilament forms above a flux cancelation neutral line at an edge of a negative-polarity network flux clump; (ii) during the minifilament's fast-eruption onset and jet-spire onset, the JBP begins brightening over the flux-cancelation neutral line. From IRIS2 inversion of the Mg II spectra, the JBP's Mg II bright plasma has electron density, temperature, and downward (red-shift) Doppler speed of 1012 cm^-3, 6000 K, and 10 kms, respectively, and the growing spire shows clockwise spin. We speculate: (i) during the slow rise of the erupting minifilament-carrying twisted flux rope, the top of the erupting flux-rope loop, by writhing, makes its field direction opposite that of encountered ambient far-reaching field; (ii) the erupting kink then can reconnect with the far-reaching field to make the spire and reconnect internally to make the JBP. We conclude that this coronal jet is normal in that magnetic flux cancelation builds a minifilament-carrying twisted flux rope and triggers the JBP-generating and jet-spire-generating eruption of the flux rope. Title: Decaying Oblique Orbits as a Hypothesis for the Origin of Nearly Horizontal Impact Craters — A Survey of Some Candidate Paterae on Mars Authors: Moore, R. B. Bibcode: 2022LPICo2702.2011M Altcode: Factors influencing the occurrence of nearly horizontal impact craters are discussed hypothetically and tested by tabulating a set of 13 such craters on Mars over 20 km long. It is observed that these have headings >35deg from the equatorial plane. Title: Bipolar Ephemeral Active Regions, Magnetic Flux Cancellation, and Solar Magnetic Explosions Authors: Moore, Ronald L.; Panesar, Navdeep K.; Sterling, Alphonse C.; Tiwari, Sanjiv K. Bibcode: 2022ApJ...933...12M Altcode: 2022arXiv220313287M We examine the cradle-to-grave magnetic evolution of 10 bipolar ephemeral active regions (BEARs) in solar coronal holes, especially aspects of the magnetic evolution leading to each of 43 obvious microflare events. The data are from the Solar Dynamics Observatory: 211 Å coronal EUV images and line-of-sight photospheric magnetograms. We find evidence that (1) each microflare event is a magnetic explosion that results in a miniature flare arcade astride the polarity inversion line (PIL) of the explosive lobe of the BEAR's anemone magnetic field; (2) relative to the BEAR's emerged flux-rope Ω loop, the anemone's explosive lobe can be an inside lobe, an outside lobe, or an inside-and-outside lobe; (3) 5 events are confined explosions, 20 events are mostly confined explosions, and 18 events are blowout explosions, which are miniatures of the magnetic explosions that make coronal mass ejections (CMEs); (4) contrary to the expectation of Moore et al., none of the 18 blowout events explode from inside the BEAR's Ω loop during the Ω loop's emergence; and (5) before and during each of the 43 microflare events, there is magnetic flux cancellation at the PIL of the anemone's explosive lobe. From finding evident flux cancellation at the underlying PIL before and during all 43 microflare events-together with BEARs evidently being miniatures of all larger solar bipolar active regions-we expect that in essentially the same way, flux cancellation in sunspot active regions prepares and triggers the magnetic explosions for many major flares and CMEs. Title: Dilution of Boundary Layer Cloud Condensation Nucleus Concentrations by Free Tropospheric Entrainment During Marine Cold Air Outbreaks Authors: Tornow, F.; Ackerman, A. S.; Fridlind, A. M.; Cairns, B.; Crosbie, E. C.; Kirschler, S.; Moore, R. H.; Painemal, D.; Robinson, C. E.; Seethala, C.; Shook, M. A.; Voigt, C.; Winstead, E. L.; Ziemba, L. D.; Zuidema, P.; Sorooshian, A. Bibcode: 2022GeoRL..4998444T Altcode: Recent aircraft measurements over the northwest Atlantic enable an investigation of how entrainment from the free troposphere (FT) impacts cloud condensation nucleus (CCN) concentrations in the marine boundary layer (MBL) during cold-air outbreaks (CAOs), motivated by the role of CCN in mediating transitions from closed to open-cell regimes. Observations compiled over eight flights indicate predominantly far lesser CCN concentrations in the FT than in the MBL. For one flight, a fetch-dependent MBL-mean CCN budget is compiled from estimates of sea-surface fluxes, entrainment of FT air, and hydrometeor collision-coalescence, based on in-situ and remote-sensing measurements. Results indicate a dominant role of FT entrainment in reducing MBL CCN concentrations, consistent with satellite-observed trends in droplet number concentration upwind of CAO cloud-regime transitions over the northwest Atlantic. Relatively scant CCN may widely be associated with FT dry intrusions, and should accelerate cloud-regime transitions where underlying MBL air is CCN-rich, thereby reducing regional albedo. Title: Homologous Compact Major Blowout-eruption Solar Flares and their Production of Broad CMEs Authors: Sahu, Suraj; Joshi, Bhuwan; Sterling, Alphonse C.; Mitra, Prabir K.; Moore, Ronald L. Bibcode: 2022ApJ...930...41S Altcode: 2022arXiv220303954S We analyze the formation mechanism of three homologous broad coronal mass ejections (CMEs) resulting from a series of solar blowout-eruption flares with successively increasing intensities (M2.0, M2.6, and X1.0). The flares originated from NOAA Active Region 12017 during 2014 March 28-29 within an interval of ≍24 hr. Coronal magnetic field modeling based on nonlinear force-free field extrapolation helps to identify low-lying closed bipolar loops within the flaring region enclosing magnetic flux ropes. We obtain a double flux rope system under closed bipolar fields for all the events. The sequential eruption of the flux ropes led to homologous flares, each followed by a CME. Each of the three CMEs formed from the eruptions gradually attained a large angular width, after expanding from the compact eruption-source site. We find these eruptions and CMEs to be consistent with the "magnetic-arch-blowout" scenario: each compact-flare blowout eruption was seated in one foot of a far-reaching magnetic arch, exploded up the encasing leg of the arch, and blew out the arch to make a broad CME. Title: Towards Equitable, Diverse, and Inclusive science collaborations: The Multimessenger Diversity Network Authors: Bechtol, E.; IceCube; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z.; Bechtol, K.; BenZvi, S.; Bleve, C.; Castro, D.; Cenko, B.; Corlies, L.; Furniss, A.; Hui, C. M.; Kaplan, D. L.; Key, J. S.; Madsen, J.; McNally, F.; McLaughlin, M.; Mukherjee, R.; Ojha, R.; Sanders, J.; Santander, M.; Schlieder, J.; Shoemaker, D. H.; Vigeland, S. Bibcode: 2022icrc.confE1383B Altcode: 2022PoS...395E1383B; 2021arXiv210712179B The Multimessenger Diversity Network (MDN), formed in 2018, extends the basic principle of multimessenger astronomy -- that working collaboratively with different approaches enhances understanding and enables previously impossible discoveries -- to equity, diversity, and inclusion (EDI) in science research collaborations. With support from the National Science Foundation INCLUDES program, the MDN focuses on increasing EDI by sharing knowledge, experiences, training, and resources among representatives from multimessenger science collaborations. Representatives to the MDN become engagement leads in their collaboration, extending the reach of the community of practice. An overview of the MDN structure, lessons learned, and how to join are presented. Title: Completing Aganta Kairos: Capturing Metaphysical Time on the Seventh Continent Authors: Madsen, J.; Mulot, L.; IceCube; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE1381M Altcode: 2022PoS...395E1381M; 2021arXiv210801687M We present an overview of the art project Aganta Kairos (To Fish the Metaphysical Time). This project celebrates the neutrino, the ghost particle, which scientists consider a cosmic messenger and the artist regards as a link between people who care about their relationship to the cosmos and question their origins. The artwork is based on a performance of celebration and seeks to build a human community that encompasses different knowledge domains and interpretations of the universe. This intersection of knowledge is realized during the performance of placing a plaque, held with witnesses, and during subsequent exhibitions. Images, sounds, videos, and sculpture testify to the diversity of approaches to questioning our origins, ranging from traditional western science to ancient shamanism. The sites were selected for their global coverage and, for the South Pole, Mediterranean, and Lake Baikal, their connection to ongoing neutrino experiments. In December 2020, a plaque was installed at the South Pole IceCube Laboratory, the seventh and final site. We provide examples of images and links to additional images and videos. Title: P-ONE second pathfinder mission: STRAW-b Authors: Rea, I. C.; Holzapfel, K.; Baron, A.; Bailly, N.; Bedard, J.; Bohmer, M.; Bosma, J.; Brussow, D.; Cheng, J.; Clark, K.; Croteau, B.; Danninger, M.; Deis, N.; Ens, M.; Fox, R.; Fruck, C.; Gartner, A.; Gernhäuser, R.; Grant, D.; He, H.; Henningsen, F.; Hotte, R.; Jenkyns, R.; Johnson, H.; Katil, A.; Kopper, C.; Krauss, C.; Kulin, I.; Leismüller, K.; Leys, S.; Lin, T. T. Y.; Macoun, P.; McElroy, T.; Meighen-Berger, S.; Michel, J.; Moore, R.; Morley, M.; Papp, L.; Pirenne, B.; Qiu, T.; Rankin, M.; Rea, I. C.; Resconi, E.; Round, A.; Ruskey, A.; Rutley, R.; Spannfellner, C.; Stacho, J.; Timmerman, R.; Tomlin, M.; Tradewell, M.; Traxler, M.; Uganecz, M.; Wagner, S.; Zheng, Y.; Yanez, J. P.; De Leo, F. Bibcode: 2022icrc.confE1092R Altcode: 2022PoS...395E1092R No abstract at ADS Title: Simulation Study of the Observed Radio Emission of Air Showers by the IceTop Surface Extension Authors: Coleman, A.; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.317C Altcode: 2021arXiv210709666C; 2022PoS...395E.317C Multi-detector observations of individual air showers are critical to make significant progress to precisely determine cosmic-ray quantities such as mass and energy of individual events and thus bring us a step forward in answering the open questions in cosmic-ray physics. An enhancement of IceTop, the surface array of the IceCube Neutrino Observatory, is currently underway and includes adding antennas and scintillators to the existing array of ice-Cherenkov tanks. The radio component will improve the characterization of the primary particles by providing an estimation of X$_\text{max}$ and a direct sampling of the electromagnetic cascade, both important for per-event mass classification. A prototype station has been operated at the South Pole and has observed showers, simultaneously, with the tanks, scintillator panels, and antennas. The observed radio signals of these events are unique as they are measured in the 70 to 350\,MHz band, higher than many other cosmic-ray experiments. We present a comparison of the detected events with the waveforms from CoREAS simulations, convoluted with the end-to-end electronics response, as a verification of the analysis chain. Using the detector response and the measurements of the prototype station as input, we update a Monte-Carlo-based study on the potential of the enhanced surface array for the hybrid detection of air showers by scintillators and radio antennas. Title: Concept Study of a Radio Array Embedded in a Deep Gen2-like Optical Array. Authors: Bishop, A.; Hokanson-Fasig, B.; Karle, A.; Lu, L.; IceCube-Gen2; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Allison, P.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Arlen, T.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Bartos, I.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bohmer, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Cataldo, M.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Clark, R.; Classen, L.; Coleman, A.; Collin, G.; Connolly, A.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; Deaconu, C.; De Clercq, C.; De Kockere, S.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Farrag, K.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gartner, A.; Gerhardt, L.; Gernhaeuser, R.; Ghadimi, A.; Giri, P.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Hallmann, S.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haugen, J.; Haungs, A.; Hauser, S.; Hebecker, D.; Heinen, D.; Helbing, K.; Hendricks, B.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, B.; Hoffmann, R.; Hoinka, T.; Holzapfel, K.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Huege, T.; Hughes, K.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kalekin, O.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Katori, T.; Katz, U.; Kauer, M.; Keivani, A.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Krauss, C.; Kravchenko, I.; Krebs, R.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; LoSecco, J.; Lozano Mariscal, C. J.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Mandalia, S.; Maris, I. C.; Marka, S.; Marka, Z.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Meyers, Z.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nelles, A.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Oberla, E.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; Omeliukh, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Papp, L.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Petersen, T.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pinfold, J.; Pittermann, M.; Pizzuto, A.; Plaisier, I.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Pyras, L.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Riegel, M.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Sandstrom, P.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Shaevitz, M. H.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smith, D.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Soldner-Rembold, S.; Southall, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Taketa, A.; Tanaka, H.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Torres, J.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Veberic, D.; Verpoest, S.; Vieregg, A. G.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weinstock, L. S.; Weiss, M.; Weldert, J.; Welling, C.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wissel, S.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wren, S.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z.; Zierke, S. Bibcode: 2022icrc.confE1182B Altcode: 2021arXiv210800283B; 2022PoS...395E1182B The IceCube Neutrino Observatory has discovered a diffuse astrophysical flux up to 10 PeV and is now planning a large extension with IceCube-Gen2, including an optical array and a large radio array at shallow depth [1]. Neutrino searches for energies >100 PeV are best done with such shallow radio detectors like the Askaryan Radio Array (ARA) or similar (buried as deep as 200 meters below the surface) as they are cheaper to deploy. This poster explores the potential of opportunistically burying radio antennas within the planned IceCube-Gen2 detector volume (between 1350 meters and 2600 meters below the surface). A hybrid detection of events in optical and radio could substantially improve the uncertainty of neutrino cascade direction as radio signals do not scatter in ice. We show the first results of simulating neutrinos from an astrophysical and a cosmogenic flux interacting with 9760 ARA-style vertically polarized radio antennas distributed evenly across 122 strings. Title: Development of a scintillation and radio hybrid detector array at the South Pole Authors: Oehler, M.; Turcotte, R.; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.225O Altcode: 2022PoS...395E.225O; 2021arXiv210709983O At the IceCube Neutrino Observatory, a Surface Array Enhancement is planned, consisting of 32 hybrid stations, placed within the current IceTop footprint. This surface enhancement will considerably increase the detection sensitivity to cosmic rays in the 100 TeV to 1 EeV primary energy range, measure the effects of snow accumulation on the existing IceTop tanks and serve as R&D for the possible future large-scale surface array of IceCube-Gen2. Each station has one central hybrid DAQ, which reads out 8 scintillation detectors and 3 radio antennas. The radio antenna SKALA-2 is used in this array due to its low-noise, high amplification and sensitivity in the 70-350 MHz frequency band. Every scintillation detector has an active area of 1.5 m$^2$ organic plastic scintillators connected by wavelength-shifting fibers, which are connected to a silicon photomultiplier. The signals from the scintillation detectors are integrated and digitized by a local custom electronics board and transferred to the central DAQ. When triggered by the scintillation detectors, the filtered and amplified analog waveforms from the radio antennas are read out and digitized by the central DAQ. A full prototype station has been developed and built and was installed at the South Pole in January 2020. It is planned to install the full array by 2026. In this contribution the hardware design of the array as well as the installation plans will be presented. Title: Another Look at Erupting Minifilaments at the Base of Solar X-Ray Polar Coronal "Standard" and "Blowout" Jets Authors: Sterling, Alphonse C.; Moore, Ronald L.; Panesar, Navdeep K. Bibcode: 2022ApJ...927..127S Altcode: 2022arXiv220112314S We examine 21 solar polar coronal jets that we identify in soft X-ray images obtained from the Hinode/X-ray telescope (XRT). We identify 11 of these as blowout jets and four as standard jets (with six uncertain), based on their X-ray-spire widths being respectively wide or narrow (compared to the jet's base) in the XRT images. From corresponding extreme ultraviolet (EUV) images from the Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA), essentially all (at least 20 of 21) of the jets are made by minifilament eruptions, consistent with other recent studies. Here, we examine the detailed nature of the erupting minifilaments (EMFs) in the jet bases. Wide-spire ("blowout") jets often have ejective EMFs, but sometimes they instead have an EMF that is mostly confined to the jet's base rather than ejected. We also demonstrate that narrow-spire ("standard") jets can have either a confined EMF, or a partially confined EMF where some of the cool minifilament leaks into the jet's spire. Regarding EMF visibility: we find that in some cases the minifilament is apparent in as few as one of the four EUV channels we examined, being essentially invisible in the other channels; thus, it is necessary to examine images from multiple EUV channels before concluding that a jet does not have an EMF at its base. The sizes of the EMFs, measured projected against the sky and early in their eruption, is 14″ ± 7″, which is within a factor of 2 of other measured sizes of coronal-jet EMFs. Title: Discrimination of Muons for Mass Composition Studies of Inclined Air Showers Detected with IceTop Authors: Balagopal V., A.; IceCube; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.212B Altcode: 2021arXiv210711293B; 2022PoS...395E.212B IceTop, the surface array of IceCube, measures air showers from cosmic rays within the energy range of 1 PeV to a few EeV and a zenith angle range of up to $\approx$ 36$^\circ$. This detector array can also measure air showers arriving at larger zenith angles at energies above 20 PeV. Air showers from lighter primaries arriving at the array will produce fewer muons when compared to heavier cosmic-ray primaries. A discrimination of these muons from the electromagnetic component in the shower can therefore allow a measurement of the primary mass. A study to discriminate muons using Monte-Carlo air showers of energies 20-100 PeV and within the zenith angular range of 45$^\circ$-60$^\circ$ will be presented. The discrimination is done using charge and time-based cuts which allows us to select muon-like signals in each shower. The methodology of this analysis, which aims at categorizing the measured air showers as light or heavy on an event-by-event basis, will be discussed. Title: Multimessenger NuEM Alerts with AMON Authors: Ayala, H.; Hawc; Abeysekara, A. U.; Albert, A.; Alfaro, R.; Alvarez, C.; Álvarez Romero, J. d. D.; Camacho, J. R. Angeles; Arteaga Velazquez, J. C.; Kollamparambil, A. B.; Avila Rojas, D. O.; Ayala Solares, H. A.; Babu, R.; Baghmanyan, V.; Barber, A. S.; Becerra Gonzalez, J.; Belmont-Moreno, E.; Berley, D.; Brisbois, C.; Caballero Mora, K. S.; Capistrán, T.; Carramiñana, A.; Casanova, S.; Chaparro-Amaro, O.; Cotti, U.; Cotzomi, J.; Coutiño de Leon, S.; de la Fuente, E.; de León, C. L.; Diaz, L.; Diaz Hernandez, R.; Díaz Vélez, J. C.; Dingus, B.; Durocher, M.; Ellsworth, R.; Engel, K.; Espinoza Hernández, M. C.; Fan, J.; Fang, K.; Fernandez Alonso, M.; Fick, B.; Fleischhack, H.; Flores, J. L.; Fraija, N. I.; Garcia Aguilar, D.; Garcia-Gonzalez, J. A.; García-Luna, J. L.; García-Torales, G.; Garfias, F.; Giacinti, G.; Goksu, H.; González, M. M.; Goodman, J. A.; Harding, J. P.; Hernández Cadena, S.; Herzog, I.; Hinton, J.; Hona, B.; Huang, D.; Hueyotl-Zahuantitla, F.; Hui, M.; Humensky, B.; Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Jhee, H.; Joshi, V.; Kieda, D.; Kunde, G. J.; Kunwar, S.; Lara, A.; Lee, J.; Lee, W. H.; Lennarz, D.; Vargas, H. Leon; Linnemann, J.; Longinotti, A. L.; Lopez-Coto, R.; Luis-Raya, G.; Lundeen, J.; Malone, K.; Marandon, V.; Martinez, O.; Martinez Castellanos, I.; Martínez Huerta, H.; Martínez-Castro, J.; Matthews, J.; McEnery, J.; Miranda-Romagnoli, P.; Morales Soto, J. A.; Moreno Barbosa, E.; Mostafa, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Olivera-Nieto, L.; Omodei, N.; Peisker, A.; Pérez Araujo, Y.; Pérez Pérez, E. G.; Rho, C. D.; Rivière, C.; Rosa-Gonzalez, D.; Ruiz-Velasco, E.; Ryan, J.; Salazar, H. I.; Salesa Greus, F.; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Serna-Franco, J.; Sinnis, G.; Smith, A. J.; Springer, W. R.; Surajbali, P.; Taboada, I.; Tanner, M.; Torres, I.; Torres Escobedo, R.; Turner, R.; Ureña-Mena, F.; Villaseñor, L.; Wang, X.; Watson, I. J.; Weisgarber, T.; Werner, F.; Willox, E.; Wood, J.; Yodh, G.; Zepeda, A.; Zhou, H.; IceCube; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.958A Altcode: 2021arXiv210804920A; 2022PoS...395E.958A The Astrophysical Multimessenger Observatory Network (AMON), has developed a real-time multi-messenger alert system. The system performs coincidence analyses of datasets from gamma-ray and neutrino detectors, making the Neutrino-Electromagnetic (NuEM) alert channel. For these analyses, AMON takes advantage of sub-threshold events, i.e., events that by themselves are not significant in the individual detectors. The main purpose of this channel is to search for gamma-ray counterparts of neutrino events. We will describe the different analyses that make up this channel and present a selection of recent results. Title: Density of GeV Muons Measured with IceTop Authors: Soldin, D.; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.342S Altcode: 2022PoS...395E.342S; 2021arXiv210709583S We present a measurement of the density of GeV muons in near-vertical air showers using three years of data recorded by the IceTop array at the South Pole. We derive the muon densities as functions of energy at reference distances of 600 m and 800 m for primary energies between 2.5 PeV and 40 PeV and between 9 PeV and 120 PeV, respectively, at an atmospheric depth of about $690\,\mathrm{g/cm}^2$. The measurements are consistent with the predicted muon densities obtained from Sibyll~2.1 assuming any physically reasonable cosmic ray flux model. However, comparison to the post-LHC models QGSJet-II.04 and EPOS-LHC shows that the post-LHC models yield a higher muon density than predicted by Sibyll 2.1 and are in tension with the experimental data for air shower energies between 2.5 PeV and 120 PeV. Title: Further Evidence for the Minifilament-eruption Scenario for Solar Polar Coronal Jets Authors: Baikie, Tomi K.; Sterling, Alphonse C.; Moore, Ronald L.; Alexander, Amanda M.; Falconer, David A.; Savcheva, Antonia; Savage, Sabrina L. Bibcode: 2022ApJ...927...79B Altcode: 2022arXiv220108882B We examine a sampling of 23 polar-coronal-hole jets. We first identified the jets in soft X-ray (SXR) images from the X-ray telescope (XRT) on the Hinode spacecraft, over 2014-2016. During this period, frequently the polar holes were small or largely obscured by foreground coronal haze, often making jets difficult to see. We selected 23 jets among those adequately visible during this period, and examined them further using Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA) 171, 193, 211, and 304 Å images. In SXRs, we track the lateral drift of the jet spire relative to the jet base's jet bright point (JBP). In 22 of 23 jets, the spire either moves away from (18 cases) or is stationary relative to (4 cases) the JBP. The one exception where the spire moved toward the JBP may be a consequence of line-of-sight projection effects at the limb. From the AIA images, we clearly identify an erupting minifilament in 20 of the 23 jets, while the remainder are consistent with such an eruption having taken place. We also confirm that some jets can trigger the onset of nearby "sympathetic" jets, likely because eruption of the minifilament field of the first jet removes magnetic constraints on the base-field region of the second jet. The propensity for spire drift away from the JBP, the identification of the erupting minifilament in the majority of jets, and the magnetic-field topological changes that lead to sympathetic jets, all support or are consistent with the minifilament-eruption model for jets. Title: Studies of a muon-based mass sensitive parameter for the IceTop surface array Authors: Kang, D.; Browne, S. A.; Haungs, A.; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.; Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen, K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A. M.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg, M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.; Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.; Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark, K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; De Clercq, C.; DeLaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; De With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.; Dujmovic, H.; Dunkman, M.; DuVernois, M.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan, K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami, S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.; Jones, B.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K. i.; Kintscher, T.; Kiryluk, J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar, J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.; Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.; Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.; Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.; Paudel, E. N.; Paul, L.; Perez de los Heros, C.; Peters, L.; Peterson, J.; Philippen, S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reichherzer, P.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M. K.; Schaufel, M.; Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer, G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yu, S.; Yuan, T.; Zhang, Z. Bibcode: 2022icrc.confE.312K Altcode: 2022PoS...395E.312K; 2021arXiv210902506K IceTop is the surface instrumentation of the IceCube Neutrino Observatory at the South Pole. It is designed to measure extensive air showers of cosmic rays in the primary energy range from PeV to EeV. Air showers induced by heavier primary particles develop earlier in the atmosphere and produce more muons observable at ground level than lighter cosmic rays with the same primary energy. Therefore, the fraction of muons to all charged particles measured by IceTop characterizes the mass of primary particles. This analysis seeks a muon-based mass sensitive parameter by using the charge signal distribution for each individual cosmic ray event. In this contribution we present the analysis method for the mass-sensitive parameter and our studies of its possible application to the measurement of cosmic ray mass composition with the IceTop surface array. Title: Birth and Evolution of a Jet-Base-Topology Solar Magnetic Field with Four Consecutive Major Flare Explosions Authors: Doran, Ilana; Panesar, Navdeep K.; Tiwari, Sanjiv; Moore, Ron; Bobra, Monica; Sterling, Alphonse Bibcode: 2021AGUFMSH35B2039D Altcode: During 2011 September 6-8, NOAA solar active region (AR) 11283 produced four consecutive major coronal mass ejections (CMEs) each with a co-produced major flare (GOES class M5.3, X2.1, X1.8, and M6.7). We examined the ARs magnetic field evolution leading to and following each of these major solar magnetic explosions. We follow flux emergence, flux cancellation and magnetic shear buildup leading to each explosion, and look for sudden flux changes and shear changes wrought by each explosion. We use AIA 193 A images and line-of-sight HMI vector magnetograms from Solar Dynamics Observatory (SDO), and SunPy, SHARPkeys, and IDL Solarsoft to prepare and analyze these data. The observed evolution of the vector field informs how magnetic field emergence and cancellation lead to and trigger the magnetic explosions, and thus informs how major CMEs and their flares are produced. We find that (1) all four flares are triggered by flux cancellation, (2) the third and fourth explosions (X1.8 and M6.7) begin with a filament eruption from the cancellation neutral line, (3) in the first and second explosions a filament erupts in the core of a secondary explosion that lags the main explosion and is probably triggered by Hudson-effect field implosion under the adjacent main exploding field, and (4) the transverse field suddenly strengthens along each main explosions underlying neutral line during the explosion, also likely due to Hudson-effect field implosion. Our observations are consistent with flux cancellation at the explosions underlying neutral line being essential in the buildup and triggering of each of the four explosions in the same way as in smaller-scale magnetic explosions that drive coronal jets. Title: Characterizing Steady and Bursty Coronal Heating of a Solar Active Region Authors: Wilkerson, Lucy; Tiwari, Sanjiv; Panesar, Navdeep K.; Moore, Ronald Bibcode: 2021AGUFMSH15E2060W Altcode: One of the biggest problems in solar physics today is our inability to explain why the solar corona is so hot. In this project, we aimed to quantify transient and background coronal heating for a given active region in order to better understand coronal heating. We used SDO/AIA data of the active region NOAA 12712 observed on May 29, 2018 over a period of 24 hours with a 3-minute cadence. We calculated FeXVIII emission (hot component of AIA 94 Å channel) by removing warm components using AIA 171 and 193 Å channels. From the maximum, minimum, and mean brightness values of each pixel over the full 24 hour period, we made maximum, minimum, and mean brightness maps. We repeated this process in moving time windows of 16 hours, 8 hours, 5 hours, 3 hours, 1 hour, and 30 minutes. We used the total luminosity for each of these maps over time to make lightcurves that show the evolution of maximum, minimum, and mean brightness over time for each running window. Finally, we took the ratio of the total maximum and total minimum luminosity to total mean luminosity, and plotted these ratios over time. The average maximum to mean ratio was 8.40±0.00, 6.36±0.46, 5.29±0.34, 4.73±0.24, 4.19±0.19, 3.21±0.17, and 2.64±0.15 and the average minimum to mean ratio was 0.053±0.00, 0.08±0.00, 0.12±0.01, 0.14±0.02, 0.17±0.02, 0.26±0.02, and 0.33±0.03 for 24h, 16h, 8h, 5h, 3h, 1h, and 30m windows, respectively. As expected, the ratio of background to mean luminosity increased as the time window decreased, and the ratio of transient to mean luminosity decreased as the time window decreased. As such, the ratio of background to mean luminosity is a new and effective technique to quantify the background intensity of the active region. Our 24h window result suggests that at most 5% of the luminosity of the AR at a given time comes from the steady background heating. This upper limit increases to 33% of the luminosity of the AR for the 30 min running window. Title: Studying Solar Active-Region Magnetic Evolution Leading to a Confined Eruption Authors: Zigament, Benjamin; Sterling, Alphonse; Moore, Ronald; Falconer, David Bibcode: 2021AGUFMSH35B2037Z Altcode: Current research suggests that there exists a continuum of solar eruptions ranging from the comparatively small, such as coronal jets, to extremely large eruptions that produce coronal mass ejections (CMEs) and solar flares, with all sharing a common triggering mechanism: a filament/flux rope eruption triggered by magnetic flux cancellation. For coronal jets the erupting "minifilaments" are of length ~10,000 km (Sterling et al. 2015, Panesar et al. 2016), while the larger eruptions are accompanied by eruptions of typical filaments of size ~several x 10^4 --- ~3x10^5 km. Sterling et al. (2018) examined this idea for two small ARs (flux ~ 2x10^21 Mx) that erupted to make CMEs. They tracked the evolution of the ARs from emergence to eruption and found eruption to occur when some of the emerged flux drifted together and underwent cancellation along the main magnetic neutral line on the interior of the AR, with eruption occurring after about 30---50% of the total flux of the respective regions canceled. Here we perform a similar study, using Solar Dynamics Observatory (SDO) AIA EUV images and SDO/HMI magnetograms, of a smaller AR (total flux <~10^21 Mx) that emerged in isolation near the neutral line in a large overarching old weak-field magnetic arcade on 2014 September 8. It produced a confined eruption (i.e., one that did not make a CME) about three days later, on September 10 near 18:45 UT. The ARs flux reached maximum about 12 hr after emergence start, and then decreased continuously, with the decrease being partly from cancellation of small flux clumps in the interior of the AR. The eruption occurred when the flux had decreased by about 20%, and was centered on the neutral line of the emerged AR, but also involved filament-holding field along some of the old arcades neutral line. That filament underwent a confined eruption as part of the overall confined eruption. The emerged ARs being inside the larger arcade, its smaller size, and its smaller amount of cancellation may be reasons why the eruption was confined, instead of being ejective and producing a CME as in the two cases of Sterling et al (2018). This work was supported by funding from NASA's HGI Program. Title: A muon-track reconstruction exploiting stochastic losses for large-scale Cherenkov detectors Authors: Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alispach, C.; Alves, A. A.; Amin, N. M.; An, R.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Argüelles, C.; Axani, S.; Bai, X.; Balagopal V., A.; Barbano, A.; Barwick, S. W.; Bastian, B.; Basu, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K. -H.; Becker Tjus, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Borowka, J.; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Browne, S.; Burgman, A.; Busse, R. S.; Campana, M. A.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B. A.; Clark, K.; Classen, L.; Coleman, A.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dave, P.; De Clercq, C.; DeLaunay, J. J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desai, A.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Díaz-Vélez, J. C.; Dujmovic, H.; Dunkman, M.; DuVernois, M. A.; Dvorak, E.; Ehrhardt, T.; Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A. T.; Filimonov, K.; Finley, C.; Fischer, L.; Fox, D.; Franckowiak, A.; Friedman, E.; Fritz, A.; Fürst, P.; K. Gaisser, T.; Gallagher, J.; Ganster, E.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Goswami, S.; Grant, D.; Grégoire, T.; Griffith, Z.; Griswold, S.; Gündüz, M.; Günther, C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Ha Minh, M.; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.; Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger, E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G. S.; Jeong, M.; Jones, B. J. P.; Joppe, R.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kin, K.; Kintscher, T.; Kiryluk, J.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.; Kowalski, M.; Krings, K.; Kurahashi, N.; Kyriacou, A.; Lagunas Gualda, C.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lazar, J. P.; Lee, J. W.; Leonard, K.; Leszczyńska, A.; Li, Y.; Liu, Q. R.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Mahn, K. B. M.; Makino, Y.; Mancina, S.; Mariş, I. C.; Maruyama, R.; Mase, K.; McNally, F.; Meagher, K.; Medina, A.; Meier, M.; Meighen-Berger, S.; Merz, J.; Micallef, J.; Mockler, D.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.; Naumann, U.; Necker, J.; Nguyễn, L. V.; Niederhausen, H.; Nisa, M. U.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Sullivan, E.; Pandya, H.; Pankova, D. V.; Park, N.; Parker, G. K.; Paudel, E. N.; Paul, L.; Pérez de los Heros, C.; Philippen, S.; Pieloth, D.; Pieper, S.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries, B.; Przybylski, G. T.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch, S.; Rhode, W.; Richman, M.; Riedel, B.; Robertson, S.; Roellinghoff, G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Saffer, J.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M.; Schaufel, M.; Schieler, H.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.; Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stürwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Twagirayezu, J. P.; Ty, B.; Unland Elorrieta, M. A.; Valtonen-Mattila, N.; Vandenbroucke, J.; van Eijk, D.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Wallace, A.; Watson, T. B.; Weaver, C.; Weigel, P.; Weindl, A.; Weiss, M. J.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.; Whelan, B. J.; Whitehorn, N.; Wiebusch, C. H.; Williams, D. R.; Wolf, M.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yoshida, S.; Yuan, T.; Zhang, Z.; IceCube collaboration Bibcode: 2021JInst..16P8034A Altcode: 2021arXiv210316931A IceCube is a cubic-kilometer Cherenkov telescope operating at the South Pole. The main goal of IceCube is the detection of astrophysical neutrinos and the identification of their sources. High-energy muon neutrinos are observed via the secondary muons produced in charge current interactions with nuclei in the ice. Currently, the best performing muon track directional reconstruction is based on a maximum likelihood method using the arrival time distribution of Cherenkov photons registered by the experiment's photomultipliers. A known systematic shortcoming of the prevailing method is to assume a continuous energy loss along the muon track. However at energies >1 TeV the light yield from muons is dominated by stochastic showers. This paper discusses a generalized ansatz where the expected arrival time distribution is parametrized by a stochastic muon energy loss pattern. This more realistic parametrization of the loss profile leads to an improvement of the muon angular resolution of up to 20% for through-going tracks and up to a factor 2 for starting tracks over existing algorithms. Additionally, the procedure to estimate the directional reconstruction uncertainty has been improved to be more robust against numerical errors. Title: A fundamental mechanism of solar eruption initiation Authors: Jiang, Chaowei; Feng, Xueshang; Liu, Rui; Yan, XiaoLi; Hu, Qiang; Moore, Ronald L.; Duan, Aiying; Cui, Jun; Zuo, Pingbing; Wang, Yi; Wei, Fengsi Bibcode: 2021NatAs...5.1126J Altcode: 2021arXiv210708204J; 2021NatAs.tmp..128J Solar eruptions are spectacular magnetic explosions in the Sun's corona, and how they are initiated remains unclear. Prevailing theories often rely on special magnetic topologies that may not generally exist in the pre-eruption source region of corona. Here, using fully three-dimensional magnetohydrodynamic simulations with high accuracy, we show that solar eruptions can be initiated in a single bipolar configuration with no additional special topology. Through photospheric shearing motion alone, an electric current sheet forms in the highly sheared core field of the magnetic arcade during its quasi-static evolution. Once magnetic reconnection sets in, the whole arcade is expelled impulsively, forming a fast-expanding twisted flux rope with a highly turbulent reconnecting region underneath. The simplicity and efficacy of this scenario argue strongly for its fundamental importance in the initiation of solar eruptions. Title: What Causes Faint Solar Coronal Jets From Emerging Flux Regions In Coronal Holes? Authors: Harden, A.; Panesar, N.; Moore, R.; Sterling, A.; Adams, M. Bibcode: 2021AAS...23821314H Altcode: Using EUV images and line-of-sight magnetograms from Solar Dynamics Observatory, we examine eight emerging bipolar magnetic regions (BMRs) in central-disk coronal holes for whether the emerging magnetic arch made any noticeable coronal jets directly, via reconnection with ambient open field as modeled by Yokoyama & Shibata (1995). During emergence, each BMR produced no obvious EUV coronal jet of normal brightness, but each produced one or more faint EUV coronal jets that are discernible in AIA 193 Å images. The spires of these jets are much fainter and usually narrower than for typical EUV jets that have been observed to be produced by minifilament eruptions in quiet regions and coronal holes. For each of 26 faint jets from the eight emerging BMRs, we examine whether the faint spire was evidently made a la Yokoyama & Shibata (1995). We find: (1) 16 of these faint spires evidently originate from sites of converging opposite-polarity magnetic flux and show base brightenings like those in minifilament-eruption-driven coronal jets, (2) the 10 other faint spires maybe were made by a burst of the external-magnetic-arcade-building reconnection of the emerging magnetic arch with the ambient open field, reconnection directly driven by the arch's emergence, but (3) none were unambiguously made by such emergence-driven reconnection. Thus, for these eight emerging BMRs, the observations indicate that emergence-driven external reconnection of the emerging magnetic arch with ambient open field at most produces a jet spire that is much fainter than in previously-reported, much more obvious coronal jets driven by minifilament eruptions. Title: Network Jets As The Driver Of Counter-streaming Flows In A Solar Filament Authors: Panesar, N. K.; Tiwari, S.; Moore, R.; Sterling, A. Bibcode: 2021AAS...23820506P Altcode: We investigate the driving mechanism of counter-streaming flows in a solar filament, using EUV images from SDO/AIA, line of sight magnetograms from SDO/HMI, IRIS SJ images, and H-alpha data from GONG. We find that: (i) persistent counter-streaming flows along adjacent threads of a small (100" long) solar filament is present; (ii) both ends of the solar filament are rooted at the edges of magnetic network flux lanes; (iii) recurrent small-scale jets (also known as network jets) occur at both ends of the filament; (iv) some of the network jets occur at the sites of flux cancelation between the majority-polarity flux and merging minority-polarity flux patches; (v) these multiple network jets clearly drive the counter-streaming flows along the adjacent threads of the solar filament for ~2 hours with an average speed of 70 km s-1; (vi) some the network jets show base brightenings, analogous to the base brightenings of coronal jets; and (vii) the filament appears wider (4") in EUV images than in H-alpha images (2.5"), consistent with previous studies. Thus, our observations show that counter-streaming flows in the filament are driven by network jets and possibly these driving network jet eruptions are prepared and triggered by flux cancelation. Title: The Missing Cool Corona In The Flat Magnetic Field Around Solar Active Regions Authors: Singh, T.; Sterling, A.; Moore, R. Bibcode: 2021AAS...23831321S Altcode: SDO/AIA images the full solar disk in several EUV bands that are each sensitive to coronal plasma emissions of one or more specific temperatures. We observe that when isolated active regions (ARs) are on the disk, full-disk images in some of the coronal EUV channels show the outskirts of the AR as a dark moat surrounding the AR. Here we present several specific examples, selected from time periods when there was only a single AR present on the disk. Visually, moats are observed to be most prominent in the AIA 171 Angstrom band, which has the most sensitivity to emission from plasma at log10 T = 5.8. By using the emission measure distribution with temperature, we find the intensity of the moat to be most depressed over the temperature range log10 T ~ 5.7-6.2 for all the cases. We argue that the dark moat exists because the pressure from the strong magnetic field that splays out from the AR presses down on underlying magnetic loops, flattening those loops — along with the lowest of the AR's own loops over the moat — to a low altitude. Those loops, which would normally emit the bulk of the 171 Angstrom emission, are restricted to heights above the surface that are too low to have 171 Angstrom emitting plasmas sustained in them, while hotter EUV-emitting plasmas are sustained in the overlying higher-altitude long AR-rooted coronal loops. This potentially explains the low-coronal-temperature dark moats surrounding the ARs. Title: On Making Magnetic-flux-rope Omega Loops For Solar Bipolar Magnetic Regions Of All Sizes By Convection Cells Authors: Moore, R.; Tiwari, S.; Panesar, N.; Sterling, A. Bibcode: 2021AAS...23831318M Altcode: This poster gives an overview of Moore, R. L., Tiwari, S. K., Panesar, N. K., & Sterling, A. C. 2020, ApJ Letters, 902:L35. We propose that the magnetic-flux-rope omega loop that emerges to become any bipolar magnetic region (BMR) is made by a convection cell of the omega-loop's size from initially horizontal magnetic field ingested through the cell's bottom. This idea is based on (1) observed characteristics of BMRs of all spans (~1000 to ~200,000 km), (2) a well-known simulation of the production of a BMR by a supergranule-sized convection cell from horizontal field placed at cell bottom, and (3) a well-known convection-zone simulation. From the observations and simulations, we (1) infer that the strength of the field ingested by the biggest convection cells (giant cells) to make the biggest BMR omega loops is ~103 G, (2) plausibly explain why the span and flux of the biggest observed BMRs are ~200,000 km and ~1022 Mx, (3) suggest how giant cells might also make "failed BMR" omega loops that populate the upper convection zone with horizontal field, from which smaller convection cells make BMR omega loops of their size, (4) suggest why sunspots observed in a sunspot cycle's declining phase tend to violate the hemispheric helicity rule, and (5) support a previously proposed amended Babcock scenario (Moore, R. L., Cirtain, J. W., & Sterling, A. C. 2016, arXiv:1606.05371) for the sunspot cycle's dynamo process. Because the proposed convection-based heuristic model for making a sunspot-BMR omega loop avoids having ~105 G field in the initial flux rope at the bottom of the convection zone, it is an appealing alternative to the present magnetic-buoyancy-based standard scenario and warrants testing by high-enough-resolution giant-cell magnetoconvection simulations. Title: Coronal-jet-producing Minifilament Eruptions As A Possible Source Of Parker Solar Probe (PSP) Switchbacks Authors: Sterling, A.; Moore, R. Bibcode: 2021AAS...23812306S Altcode: The Parker Solar Probe (PSP) has observed copious rapid magnetic field direction changes in the near-Sun solar wind. These features have been called "switchbacks," and their origin is a mystery. But their widespread nature suggests that they may be generated by a frequently occurring process in the Sun's atmosphere. We examine the possibility that the switchbacks originate from coronal jets. Recent work suggests that many coronal jets result when photospheric magnetic flux cancels, and forms a small-scale "minifilament" flux rope that erupts and reconnects with coronal field. We argue that the reconnected erupting minifilament flux rope can manifest as an outward propagating Alfvenic fluctuation that steepens into an increasingly compact disturbance as it moves through the solar wind. Using previous observed properties of coronal jets that connect to coronagraph-observed white-light jets (a.k.a. "narrow CMEs"), along with typical solar wind speed values, we expect the coronal-jet-produced disturbances to traverse near-perihelion PSP in less than or about 25 min, with a velocity of about 400 km/s. To consider further the plausibility of this idea, we show that a previously studied series of equatorial latitude coronal jets, originating from the periphery of an active region, generate white-light jets in the outer corona (seen in STEREO/COR2 coronagraph images; 2.5 — 15 solar radii), and into the inner heliosphere (seen in STEREO/Hi1 heliospheric imager images; 15 — 84 solar radii). Thus it is tenable that disturbances put onto open coronal magnetic field lines by coronal-jet-producing erupting minifilament flux ropes can propagate out to PSP space and appear as switchbacks. This work was supported by the NASA Heliophysics Division, and by the NASA/MSFC Hinode Project. For further details see Sterling & Moore (2020, ApJ, 896, L18). Title: What Percentage Of The Brightest Coronal Loops Are Rooted In Mixed-polarity Magnetic Flux? Authors: Tiwari, S. K.; Evans, C. L.; Panesar, N.; Prasad, A.; Moore, R. Bibcode: 2021AAS...23820502T Altcode: We have previously shown (Tiwari et al. 2017, ApJ Letters, 843, L20) that the heating in active region (AR) coronal loops depends systematically on their photospheric magnetic setting. There, we found that the brightest and hottest loops of ARs are the ones connecting sunspot umbra/penumbra at one end to (a) penumbra, (b) unipolar plage, or (c) mixed-polarity plage on the other end. The coolest loops are the ones that connect sunspot umbra at both ends. In this work we study the brightest loops during 24 hours in the core of the active region that was observed by Hi-C 2.1. These loops have neither foot in sunspot umbra or penumbra, but in plage. We investigate what percentage of the brightest coronal loops (in SDO/AIA Fe XVIII emission) have mixed-polarity magnetic flux at least at one of their feet, and so the heating could be driven by magnetic flux cancellation. We confirm the footpoint locations of loops via non-force-free field extrapolations (using SDO/HMI magnetograms) and find that ∼40% of the loops have both feet in unipolar flux, and ∼60% of the loops have at least one foot in mixed-polarity flux. The loops having mixed-polarity foot-point flux are ∼15% longer lived on average than the ones with both feet unipolar, but their peak-intensity averages do not show any significant difference. While the presence of mixed-polarity magnetic flux at least at one foot in majority of loops strongly supports the cancellation idea, the absence of mixed-polarity magnetic flux (to the detection limit of HMI) in about 40% of the loops suggests cancellation may not be necessary for heating coronal loops, but rather might enhance heating by some factor. We will further discuss some points that support, and some points that challenge, the flux cancellation idea of coronal heating. Title: What Causes Faint Solar Coronal Jets from Emerging Flux Regions in Coronal Holes? Authors: Harden, Abigail R.; Panesar, Navdeep K.; Moore, Ronald L.; Sterling, Alphonse C.; Adams, Mitzi L. Bibcode: 2021ApJ...912...97H Altcode: 2021arXiv210307813H Using EUV images and line-of-sight magnetograms from Solar Dynamics Observatory, we examine eight emerging bipolar magnetic regions (BMRs) in central-disk coronal holes for whether the emerging magnetic arch made any noticeable coronal jets directly, via reconnection with ambient open field as modeled by Yokoyama & Shibata. During emergence, each BMR produced no obvious EUV coronal jet of normal brightness, but each produced one or more faint EUV coronal jets that are discernible in AIA 193 Å images. The spires of these jets are much fainter and usually narrower than for typical EUV jets that have been observed to be produced by minifilament eruptions in quiet regions and coronal holes. For each of 26 faint jets from the eight emerging BMRs, we examine whether the faint spire was evidently made a la Yokoyama & Shibata. We find that (1) 16 of these faint spires evidently originate from sites of converging opposite-polarity magnetic flux and show base brightenings like those in minifilament-eruption-driven coronal jets, (2) the 10 other faint spires maybe were made by a burst of the external-magnetic-arcade-building reconnection of the emerging magnetic arch with the ambient open field, with reconnection directly driven by the arch's emergence, but (3) none were unambiguously made by such emergence-driven reconnection. Thus, for these eight emerging BMRs, the observations indicate that emergence-driven external reconnection of the emerging magnetic arch with ambient open field at most produces a jet spire that is much fainter than in previously reported, much more obvious coronal jets driven by minifilament eruptions. Title: A Fundamental Mechanism of Solar Eruption Initiation Authors: Jiang, Chaowei; Feng, Xueshang; Liu, Rui; Yan, Xiaoli; Hu, Qiang; Moore, Ronald L. Bibcode: 2021EGUGA..2310493J Altcode: Solar eruptions are spectacular magnetic explosions in the Sun's corona and how they are initiated remains unclear. Prevailing theories often rely on special magnetic topologies, such as magnetic flux rope and magnetic null point, which, however, may not generally exist in the pre-eruption source region of corona. Here using fully three-dimensional magnetohydrodynamic simulations with high accuracy, we show that solar eruption can be initiated in a single bipolar configuration with no additional special topology. Through photospheric shearing motion alone, an electric current sheet forms in the highly sheared core field of the magnetic arcade during its quasi-static evolution. Once magnetic reconnection sets in, the whole arcade is expelled impulsively, forming a fast-expanding twisted flux rope with a highly turbulent reconnecting region underneath. The simplicity and efficacy of this scenario argue strongly for its fundamental importance in the initiation of solar eruptions. Title: Airborne Measurements of Contrail Ice Properties—Dependence on Temperature and Humidity Authors: Bräuer, T.; Voigt, C.; Sauer, D.; Kaufmann, S.; Hahn, V.; Scheibe, M.; Schlager, H.; Diskin, G. S.; Nowak, J. B.; DiGangi, J. P.; Huber, F.; Moore, R. H.; Anderson, B. E. Bibcode: 2021GeoRL..4892166B Altcode: The largest share in the climate impact of aviation results from contrail cirrus clouds. Here, the dependence of microphysical contrail ice properties and extinction on temperature and humidity is investigated. Contrail measurements were performed at various altitudes during the 2018 ECLIF II/NDMAX campaign with the NASA DC 8 chasing the DLR A320. Ice number concentrations and contrail extinction coefficients are largest at altitudes near 9.5 km, typical for short and medium range air traffic. At higher altitudes near 11.5 km, low ambient water vapor concentrations lead to smaller contrail particle sizes and lower extinction coefficients. In addition, contrails were detected below 8.2 km near the Schmidt Appleman contrail formation threshold temperature. Here, only a small fraction (<15%) of the emitted soot particles were activated into ice. Our observations enhance the understanding of contrail formation near the formation threshold and give a glimpse on the altitude dependence of climate relevant contrail properties. Title: The Missing Cool Corona in the Flat Magnetic Field around Solar Active Regions Authors: Singh, Talwinder; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2021ApJ...909...57S Altcode: 2020arXiv201215406S Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) images the full solar disk in several extreme-ultraviolet (EUV) bands that are each sensitive to coronal plasma emissions of one or more specific temperatures. We observe that when isolated active regions (ARs) are on the disk, full-disk images in some of the coronal EUV channels show the outskirts of the AR as a dark moat surrounding the AR. Here we present seven specific examples, selected from time periods when there was only a single AR present on the disk. Visually, we observe the moat to be most prominent in the AIA 171 Å band, which has the most sensitivity to emission from plasma at log10 T = 5.8. By examining the 1D line-of-sight emission measure temperature distribution found from six AIA EUV channels, we find the intensity of the moat to be most depressed over the temperature range log10 T ≍ 5.7-6.2 for most of the cases. We argue that the dark moat exists because the pressure from the strong magnetic field that splays out from the AR presses down on underlying magnetic loops, flattening those loops—along with the lowest of the AR's own loops over the moat—to a low altitude. Those loops, which would normally emit the bulk of the 171 Å emission, are restricted to heights above the surface that are too low to have 171 Å emitting plasmas sustained in them, according to Antiochos & Noci, while hotter EUV-emitting plasmas are sustained in the overlying higher-altitude long AR-rooted coronal loops. This potentially explains the low-coronal-temperature dark moats surrounding the ARs. Title: Are the Brightest Coronal Loops Always Rooted in Mixed-polarity Magnetic Flux? Authors: Tiwari, Sanjiv K.; Evans, Caroline L.; Panesar, Navdeep K.; Prasad, Avijeet; Moore, Ronald L. Bibcode: 2021ApJ...908..151T Altcode: 2021arXiv210210146T A recent study demonstrated that freedom of convection and strength of magnetic field in the photospheric feet of active-region (AR) coronal loops, together, can engender or quench heating in them. Other studies stress that magnetic flux cancellation at the loop-feet potentially drives heating in loops. We follow 24 hr movies of a bipolar AR, using extreme ultraviolet images from the Atmospheric Imaging Assembly/Solar Dynamics Observatory (SDO) and line-of-sight (LOS) magnetograms from the Helioseismic and Magnetic Imager (HMI)/SDO, to examine magnetic polarities at the feet of 23 of the brightest coronal loops. We derived Fe XVIII emission (hot-94) images (using the Warren et al. method) to select the hottest/brightest loops, and confirm their footpoint locations via non-force-free field extrapolations. From 6″ × 6″ boxes centered at each loop foot in LOS magnetograms we find that ∼40% of the loops have both feet in unipolar flux, and ∼60% of the loops have at least one foot in mixed-polarity flux. The loops with both feet unipolar are ∼15% shorter lived on average than the loops having mixed-polarity foot-point flux, but their peak-intensity averages are equal. The presence of mixed-polarity magnetic flux in at least one foot in the majority of the loops suggests that flux cancellation at the footpoints may drive most of the heating. But the absence of mixed-polarity magnetic flux (to the detection limit of HMI) in ∼40% of the loops suggests that flux cancellation may not be necessary to drive heating in coronal loops—magnetoconvection and field strength at both loop feet possibly drive much of the heating, even in the cases where a loop foot presents mixed-polarity magnetic flux. Title: Fine-scale explosive energy release at sites of magnetic flux cancellation in the core of a solar active region: Hi-C 2.1, IRIS and SDO observations Authors: Tiwari, Sanjiv Kumar; Moore, Ronald; De Pontieu, Bart; Winebarger, Amy; Panesar, Navdeep Kaur Bibcode: 2021cosp...43E1779T Altcode: The second sounding-rocket flight of the High-Resolution Coronal Imager (Hi-C 2.1) provided unprecedentedly-high spatial and temporal resolution (~250 km, 4.4 s) coronal EUV images of Fe IX/X emission at 172 A, of a solar active region (AR NOAA 12712) near solar disk center. Three morphologically-different types (I: dot-like, II: loop-like, & III: surge/jet-like) of fine-scale sudden brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. Although type Is resemble IRIS bombs (in size, and brightness with respect to surroundings), our dot-like events are apparently much hotter, and shorter in span (70 s). Because Dot-like brightenings are not as clearly discernible in AIA 171 A as in Hi-C 172 A, they were not reported before. We complement the 5-minute-duration Hi-C 2.1 data with SDO/HMI magnetograms, SDO/AIA EUV and UV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying flux cancellation at the microflare's polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. In types I and II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow. The light curves from Hi-C, AIA and IRIS peak nearly simultaneously for many of these events and none of the events display a systematic cooling sequence as seen in typical coronal flares, suggesting that these tiny brightening events have chromospheric/transition-region origin. Title: Coronal Jets Observed at Sites of Magnetic Flux Cancelation Authors: Panesar, Navdeep Kaur; Sterling, Alphonse; Moore, Ronald; Tiwari, Sanjiv Kumar Bibcode: 2021cosp...43E1783P Altcode: Solar jets of all sizes are magnetically channeled narrow eruptive events; the larger ones are often observed in the solar corona in EUV and coronal X-ray images. Recent observations show that the buildup and triggering of the minifilament eruptions that drive coronal jets result from magnetic flux cancelation under the minifilament, at the neutral line between merging majority-polarity and minority-polarity magnetic flux patches. Here we investigate the magnetic setting of on-disk small-scale jets (also known as jetlets) by using high resolution 172A images from the High-resolution Coronal Imager (Hi-C2.1) and EUV images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), and UV images from the Interface Region Imaging Spectrograph (IRIS), and line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). We observe jetlets at edges of magnetic network lanes. From magnetograms co-aligned with the Hi-C, IRIS, and AIA images, we find that the jetlets stem from sites of flux cancelation between merging majority-polarity and minority-polarity flux patches, and some of the jetlets show faint brightenings at their bases reminiscent of the base brightenings in coronal jets. Based on these observations of jetlets and our previous observations of ∼90 coronal jets in quiet regions and coronal holes, we infer that flux cancelation is the essential process in the buildup and triggering of jetlets. Our observations suggest that network jetlet eruptions are small-scale analogs of both larger-scale coronal jet eruptions and the still-larger-scale eruptions that make major CMEs. Title: The Signature of Sulfur: Geochemical Characterization of Hydrothermal S-rich Deposits in Terrestrial Mars Analogs Authors: Moore, R.; Ende, J. J.; Burtt, P. K.; Szynkiewicz, A. Bibcode: 2020AGUFMEP017..11M Altcode: The Spirit rover found localized hydrothermal/fumarolic deposits enriched in Fe-, Ca-, and Mg-sulfate within Gusev crater. However, it did not find conclusive evidence for the presence of reduced S (e.g., sulfides, elemental S), which dominates analogous terrestrial hydrothermal settings. Consequently, the sulfate (SO4) enrichment and apparent absence of reduced S in Gusev sediments raises questions about the formation and oxidation mechanisms of S in acidic hydrothermal systems. To address these questions, we collected sediment and water samples from highly-acidic hot springs, mud pots, fumaroles, and drainages with elevated H2S emissions in four analog sites, including Yellowstone, Valles Caldera, Lassen, and Iceland. The method of Sulfur Sequential Extraction (SSE) was used to determine oxidation states and measure quantities and S isotope compositions of sulfides (S2-, S-), elemental S (S0), and sulfates (S6+). Results show that S0 was highly abundant in most sediment samples (0.3 - 20 wt.% S, but up to ~70 wt.% S), followed by S- (0.2 - 4.4 wt.% S), with significantly lower S6+ in the sediment and water column (0.07 - 1.6 wt.% S). In the majority of samples, the δ34S of S6+ was lower (-3 to +3‰) compared to emitted H2S (-2 to +6‰), but similar to S- and S0 precipitated in the hydrothermal sediments (-7 to +3‰), suggesting the importance of subsequent step-oxidation of the reduced S to sulfate. Our results indicate that surface hydrothermal systems are capable of producing large quantities of reduced S, and could explain high-S deposits on Mars. However, the reported S contents for Gusev crater are lower in range (0.4 - 5.6 wt.% S) and more oxidized (mainly sulfate) compared to the studied analog sites (0.2 - 24 wt.% S, mainly elemental S and sulfides). The negligible amounts of reduced S in Gusev may be a result of subsequent oxidation to SO4, and the overall smaller amount of S might reflect removal of SO4 by an active hydrological cycle during formation or later on over several billion years. Our previous study showed that ferric iron (Fe3+) reduction participates in the step-oxidation of hydrothermal H2S. This is especially compelling given the high concentrations of Fe3+ iron and Fe-sulfates detected in Gusev, and thus provides new context for the formation of sulfate in Martian oxygen-depleted surface environments. Title: Fine-scale explosive energy release at sites of magnetic flux cancellation in the core of a solar active region: Hi-C 2.1, IRIS and SDO observations Authors: Tiwari, S. K.; Panesar, N. K.; Moore, R. L.; De Pontieu, B.; Winebarger, A. R. Bibcode: 2020AGUFMSH0010007T Altcode: The second sounding-rocket flight of the High-Resolution Coronal Imager (Hi-C 2.1) provided unprecedentedly-high spatial and temporal resolution (~250 km, 4.4 s) coronal EUV images of Fe IX/X emission at 172 Å, of a solar active region (AR NOAA 12712) near solar disk center. Three morphologically-different types (I: dot-like, II: loop-like, & III: surge/jet-like) of fine-scale sudden brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. Although type Is resemble IRIS bombs (in size, and brightness with respect to surroundings), our dot-like events are apparently much hotter, and shorter in span (70 s). Because Dot-like brightenings are not as clearly discernible in AIA 171 Å as in Hi-C 172 Å, they were not reported before. We complement the 5-minute-duration Hi-C 2.1 data with SDO/HMI magnetograms, SDO/AIA EUV and UV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying flux cancellation at the microflare's polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. In types I and II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow. The light curves from Hi-C, AIA and IRIS peak nearly simultaneously for many of these events and none of the events display a systematic cooling sequence as seen in typical coronal flares, suggesting that these tiny brightening events have chromospheric/transition-region origin. Title: Cosmic ray spectrum from 250 TeV to 10 PeV using IceTop Authors: Aartsen, M. G.; Abbasi, R.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alispach, C.; Amin, N. M.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Argüelles, C.; Auffenberg, J.; Axani, S.; Bagherpour, H.; Bai, X.; Balagopal V., A.; Barbano, A.; Barwick, S. W.; Bastian, B.; Baum, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K. -H.; Becker Tjus, J.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bohm, C.; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Burgman, A.; Buscher, J.; Busse, R. S.; Carver, T.; Chen, C.; Cheung, E.; Chirkin, D.; Choi, S.; Clark, B. A.; Clark, K.; Classen, L.; Coleman, A.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dave, P.; De Clercq, C.; DeLaunay, J. J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Dharani, S.; Diaz, A.; Díaz-Vélez, J. C.; Dujmovic, H.; Dvorak, E.; Eberhardt, B.; Ehrhardt, T.; Eller, P.; Engel, R.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Fienberg, A. T.; Filimonov, K.; Finley, C.; Fox, D.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garrappa, S.; Gerhardt, L.; Ghorbani, K.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Grégoire, T.; Griffith, Z.; Griswold, S.; Günder, M.; Gündüz, M.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Hanson, K.; Haungs, A.; Hauser, S.; Hebecker, D.; Heereman, D.; Heix, P.; Helbing, K.; Hellauer, R.; Henningsen, F.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huber, M.; Huber, T.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.; Jonske, F.; Joppe, R.; Kang, D.; Kang, W.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kowalski, M.; Krings, K.; Krückl, G.; Kulacz, N.; Kurahashi, N.; Kyriacou, A.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lazar, J. P.; Leonard, K.; Leszczyńska, A.; Li, Y.; Liu, Q. R.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Ludwig, A.; Lünemann, J.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Mallik, P.; Mallot, K.; Mancina, S.; Mariş, I. C.; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Medina, A.; Meier, M.; Meighen-Berger, S.; Merino, G.; Merz, J.; Meures, T.; Micallef, J.; Mockler, D.; Momenté, G.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, M.; Muth, P.; Nagai, R.; Naumann, U.; Neer, G.; Nguyën, L. V.; Niederhausen, H.; Nisa, M. U.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Murchadha, A.; O'Sullivan, E.; Pandya, H.; Pankova, D. V.; Park, N.; Parker, G. K.; Paudel, E. N.; Peiffer, P.; Pérez de los Heros, C.; Philippen, S.; Pieloth, D.; Pieper, S.; Pinat, E.; Pizzuto, A.; Plum, M.; Popovych, Y.; Porcelli, A.; Price, P. B.; Przybylski, G. T.; Raab, C.; Raissi, A.; Rameez, M.; Rauch, L.; Rawlins, K.; Rea, I. C.; Rehman, A.; Reimann, R.; Relethford, B.; Renschler, M.; Renzi, G.; Resconi, E.; Rhode, W.; Richman, M.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.; Safa, I.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Scharf, M.; Schaufel, M.; Schieler, H.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L.; Sclafani, S.; Seckel, D.; Seunarine, S.; Shefali, S.; Silva, M.; Smithers, B.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Strotjohann, N. L.; Stürwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tilav, S.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Ty, B.; Unger, E.; Unland Elorrieta, M. A.; Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijk, D.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Watson, T. B.; Weaver, C.; Weindl, A.; Weldert, J.; Wendt, C.; Werthebach, J.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woschnagg, K.; Wrede, G.; Wulff, J.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Yuan, T.; Zhang, Z.; Zöcklein, M.; IceCube Collaboration Bibcode: 2020PhRvD.102l2001A Altcode: 2020arXiv200605215I We report here an extension of the measurement of the all-particle cosmic-ray spectrum with IceTop to lower energy. The new measurement gives full coverage of the knee region of the spectrum and reduces the gap in energy between previous IceTop and direct measurements. With a new trigger that selects events in closely spaced detectors in the center of the array, the IceTop energy threshold is lowered by almost an order of magnitude below its previous threshold of 2 PeV. In this paper we explain how the new trigger is implemented, and we describe the new machine-learning method developed to deal with events with very few detectors hit. We compare the results with previous measurements by IceTop and others that overlap at higher energy and with HAWC and Tibet in the 100 TeV range. Title: Network Jets as the Driver of Counter-streaming Flows in a Solar Filament Authors: Panesar, N. K.; Tiwari, S. K.; Moore, R. L.; Sterling, A. C. Bibcode: 2020AGUFMSH0240004P Altcode: We investigate the driving mechanism of counter-streaming flows in a solar filament, using EUV images from SDO/AIA, line of sight magnetograms from SDO/HMI, IRIS SJ images, and H-alpha data from GONG. We find that: (i) persistent counter-streaming flows along adjacent threads of a small (100" long) solar filament is present; (ii) both ends of the solar filament are rooted at the edges of magnetic network flux lanes; (iii) recurrent small-scale jets (also known as network jets) occur at both ends of the filament; (iv) some of the network jets occur at the sites of flux cancelation between the majority-polarity flux and merging minority-polarity flux patches; (v) these multiple network jets clearly drive the counter-streaming flows along the adjacent threads of the solar filament for ~2 hours with an average speed of 70 km s-1; (vi) some the network jets show base brightenings, analogous to the base brightenings of coronal jets; and (vii) the filament appears wider (4") in EUV images than in H-alpha images (2.5"), consistent with previous studies. Thus, our observations show that counter-streaming flows in the filament are driven by network jets and possibly these driving network jet eruptions are prepared and triggered by flux cancelation. Title: Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections Authors: Patsourakos, S.; Vourlidas, A.; Török, T.; Kliem, B.; Antiochos, S. K.; Archontis, V.; Aulanier, G.; Cheng, X.; Chintzoglou, G.; Georgoulis, M. K.; Green, L. M.; Leake, J. E.; Moore, R.; Nindos, A.; Syntelis, P.; Yardley, S. L.; Yurchyshyn, V.; Zhang, J. Bibcode: 2020SSRv..216..131P Altcode: 2020arXiv201010186P A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multi-height vector magnetic field measurements is the optimal approach for resolving the issue conclusively. We demonstrate the approach using MHD simulations and synthetic coronal images. Title: On Making Magnetic-flux-rope Ω Loops for Solar Bipolar Magnetic Regions of All Sizes by Convection Cells Authors: Moore, Ronald L.; Tiwari, Sanjiv K.; Panesar, Navdeep K.; Sterling, Alphonse C. Bibcode: 2020ApJ...902L..35M Altcode: 2020arXiv200913694M We propose that the flux-rope Ω loop that emerges to become any bipolar magnetic region (BMR) is made by a convection cell of the Ω-loop's size from initially horizontal magnetic field ingested through the cell's bottom. This idea is based on (1) observed characteristics of BMRs of all spans (∼1000 to ∼200,000 km), (2) a well-known simulation of the production of a BMR by a supergranule-sized convection cell from horizontal field placed at cell bottom, and (3) a well-known convection-zone simulation. From the observations and simulations, we (1) infer that the strength of the field ingested by the biggest convection cells (giant cells) to make the biggest BMR Ω loops is ∼103 G, (2) plausibly explain why the span and flux of the biggest observed BMRs are ∼200,000 km and ∼1022 Mx, (3) suggest how giant cells might also make "failed-BMR" Ω loops that populate the upper convection zone with horizontal field, from which smaller convection cells make BMR Ω loops of their size, (4) suggest why sunspots observed in a sunspot cycle's declining phase tend to violate the hemispheric helicity rule, and (5) support a previously proposed amended Babcock scenario for the sunspot cycle's dynamo process. Because the proposed convection-based heuristic model for making a sunspot-BMR Ω loop avoids having ∼105 G field in the initial flux rope at the bottom of the convection zone, it is an appealing alternative to the present magnetic-buoyancy-based standard scenario and warrants testing by high-enough-resolution giant-cell magnetoconvection simulations. Title: Possible Evolution of Minifilament-Eruption-Produced Solar Coronal Jets, Jetlets, and Spicules, into Magnetic-Twist-Wave “Switchbacks” Observed by the Parker Solar Probe (PSP) Authors: Sterling, Alphonse C.; Moore, Ronald L.; Panesar, Navdeep K.; Samanta, Tanmoy Bibcode: 2020JPhCS1620a2020S Altcode: 2020arXiv201012991S Many solar coronal jets result from erupting miniature-filament (“minifilament”) magnetic flux ropes that reconnect with encountered surrounding far-reaching field. Many of those minifilament flux ropes are apparently built and triggered to erupt by magnetic flux cancelation. If that cancelation (or some other process) results in the flux rope’s field having twist, then the reconnection with the far-reaching field transfers much of that twist to that reconnected far-reaching field. In cases where that surrounding field is open, the twist can propagate to far distances from the Sun as a magnetic-twist Alfvénic pulse. We argue that such pulses from jets could be the kinked-magnetic-field structures known as “switchbacks,” detected in the solar wind during perihelion passages of the Parker Solar Probe (PSP). For typical coronal-jet-generated Alfvénic pulses, we expect that the switchbacks would flow past PSP with a duration of several tens of minutes; larger coronal jets might produce switchbacks with passage durations ∼1hr. Smaller-scale jet-like features on the Sun known as “jetlets” may be small-scale versions of coronal jets, produced in a similar manner as the coronal jets. We estimate that switchbacks from jetlets would flow past PSP with a duration of a few minutes. Chromospheric spicules are jet-like features that are even smaller than jetlets. If some portion of their population are indeed very-small-scale versions of coronal jets, then we speculate that the same processes could result in switchbacks that pass PSP with durations ranging from about ∼2 min down to tens of seconds. Title: Sequential Lid Removal in a Triple-decker Chain of CME-producing Solar Eruptions Authors: Joshi, Navin Chandra; Sterling, Alphonse C.; Moore, Ronald L.; Joshi, Bhuwan Bibcode: 2020ApJ...901...38J Altcode: 2020arXiv200804525J We investigate the onsets of three consecutive coronal mass ejection (CME) eruptions in 12 hr from a large bipolar active region (AR) observed by the Solar Dynamics Observatory (SDO), the Solar Terrestrial Relations Observatory (STEREO), the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), and the Geostationary Operational Environmental Satellite (GOES). Evidently, the AR initially had a "triple-decker" configuration: three flux ropes in a vertical stack above the polarity inversion line (PIL). Upon being bumped by a confined eruption of the middle flux rope, the top flux rope erupts to make the first CME and its accompanying AR-spanning flare arcade rooted in a far apart pair of flare ribbons. The second CME is made by eruption of the previously arrested middle flux rope, which blows open the flare arcade of the first CME and produces a flare arcade rooted in a pair of flare ribbons closer to the PIL than those of the first CME. The third CME is made by blowout eruption of the bottom flux rope, which blows open the second flare arcade and makes its own flare arcade and pair of flare ribbons. Flux cancellation observed at the PIL likely triggers the initial confined eruption of the middle flux rope. That confined eruption evidently triggers the first CME eruption. The lid-removal mechanism instigated by the first CME eruption plausibly triggers the second CME eruption. Further lid removal by the second CME eruption plausibly triggers the final CME eruption. Title: Network Jets as the Driver of Counter-streaming Flows in a Solar Filament/Filament Channel Authors: Panesar, Navdeep K.; Tiwari, Sanjiv K.; Moore, Ronald L.; Sterling, Alphonse C. Bibcode: 2020ApJ...897L...2P Altcode: 2020arXiv200604249P Counter-streaming flows in a small (100″ long) solar filament/filament channel are directly observed in high-resolution Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) extreme-ultraviolet (EUV) images of a region of enhanced magnetic network. We combine images from SDO/AIA, SDO/Helioseismic and Magnetic Imager (HMI), and the Interface Region Imaging Spectrograph (IRIS) to investigate the driving mechanism of these flows. We find that: (I) counter-streaming flows are present along adjacent filament/filament channel threads for ∼2 hr, (II) both ends of the filament/filament channel are rooted at the edges of magnetic network flux lanes along which there are impinging fine-scale opposite-polarity flux patches, (III) recurrent small-scale jets (known as network jets) occur at the edges of the magnetic network flux lanes at the ends of the filament/filament channel, (IV) the recurrent network jet eruptions clearly drive the counter-streaming flows along threads of the filament/filament channel, (V) some of the network jets appear to stem from sites of flux cancelation, between network flux and merging opposite-polarity flux, and (VI) some show brightening at their bases, analogous to the base brightening in coronal jets. The average speed of the counter-streaming flows along the filament/filament channel threads is 70 km s-1. The average widths of the AIA filament/filament channel and the Hα filament are 4″ and 2"5, respectively, consistent with the earlier findings that filaments in EUV images are wider than in Hα images. Thus, our observations show that the continually repeated counter-streaming flows come from network jets, and these driving network jet eruptions are possibly prepared and triggered by magnetic flux cancelation. Title: Coronal-jet-producing Minifilament Eruptions as a Possible Source of Parker Solar Probe Switchbacks Authors: Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2020ApJ...896L..18S Altcode: 2020arXiv200604990S The Parker Solar Probe (PSP) has observed copious rapid magnetic field direction changes in the near-Sun solar wind. These features have been called "switchbacks," and their origin is a mystery. But their widespread nature suggests that they may be generated by a frequently occurring process in the Sun's atmosphere. We examine the possibility that the switchbacks originate from coronal jets. Recent work suggests that many coronal jets result when photospheric magnetic flux cancels, and forms a small-scale "minifilament" flux rope that erupts and reconnects with coronal field. We argue that the reconnected erupting-minifilament flux rope can manifest as an outward propagating Alfvénic fluctuation that steepens into an increasingly compact disturbance as it moves through the solar wind. Using previous observed properties of coronal jets that connect to coronagraph-observed white-light jets (a.k.a. "narrow CMEs"), along with typical solar wind speed values, we expect the coronal-jet-produced disturbances to traverse near-perihelion PSP in ≲25 minutes, with a velocity of ∼400 km s-1. To consider further the plausibility of this idea, we show that a previously studied series of equatorial latitude coronal jets, originating from the periphery of an active region, generate white-light jets in the outer corona (seen in STEREO/COR2 coronagraph images; 2.5-15 R⊙), and into the inner heliosphere (seen in Solar-Terrestrial Relations Observatory (STEREO)/Hi1 heliospheric imager images; 15-84 R⊙). Thus it is tenable that disturbances put onto open coronal magnetic field lines by coronal-jet-producing erupting-minifilament flux ropes can propagate out to PSP space and appear as switchbacks. Title: Onset of Magnetic Explosion in Solar Coronal Jets in Quiet Regions on the Central Disk Authors: Panesar, Navdeep K.; Moore, Ronald L.; Sterling, Alphonse C. Bibcode: 2020ApJ...894..104P Altcode: 2020arXiv200604253P We examine the initiation of 10 coronal jet eruptions in quiet regions on the central disk, thereby avoiding near-limb spicule-forest obscuration of the slow-rise onset of the minifilament eruption. From the Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å 12 s cadence movie of each eruption, we (1) find and compare the start times of the minifilament's slow rise, the jet-base bright point, the jet-base-interior brightening, and the jet spire, and (2) measure the minifilament's speed at the start and end of its slow rise. From (a) these data, (b) prior observations showing that each eruption was triggered by magnetic flux cancelation under the minifilament, and (c) the breakout-reconnection current sheet observed in one eruption, we confirm that quiet-region jet-making minifilament eruptions are miniature versions of CME-making filament eruptions, and surmise that in most quiet-region jets: (1) the eruption starts before runaway reconnection starts, (2) runaway reconnection does not start until the slow-rise speed is at least ∼1 km s-1, and (3) at and before eruption onset, there is no current sheet of appreciable extent. We therefore expect that (I) many CME-making filament eruptions are triggered by flux cancelation under the filament, (II) emerging bipoles seldom, if ever, directly drive jet production because the emergence is seldom, if ever, fast enough, and (III) at a separatrix or quasi-separatrix in any astrophysical setting of a magnetic field in low-beta plasma, a current sheet of appreciable extent can be built only dynamically by a magnetohydrodynamic convulsion of the field, not by quasi-static gradual converging of the field. Title: A Solar Magnetic-fan Flaring Arch Heated by Nonthermal Particles and Hot Plasma from an X-Ray Jet Eruption Authors: Lee, Kyoung-Sun; Hara, Hirohisa; Watanabe, Kyoko; Joshi, Anand D.; Brooks, David H.; Imada, Shinsuke; Prasad, Avijeet; Dang, Phillip; Shimizu, Toshifumi; Savage, Sabrina L.; Moore, Ronald; Panesar, Navdeep K.; Reep, Jeffrey W. Bibcode: 2020ApJ...895...42L Altcode: 2020arXiv200509875L We have investigated an M1.3 limb flare, which develops as a magnetic loop/arch that fans out from an X-ray jet. Using Hinode/EIS, we found that the temperature increases with height to a value of over 107 K at the loop top during the flare. The measured Doppler velocity (redshifts of 100-500 km s-1) and the nonthermal velocity (≥100 km s-1) from Fe XXIV also increase with loop height. The electron density increases from 0.3 × 109 cm-3 early in the flare rise to 1.3 × 109 cm-3 after the flare peak. The 3D structure of the loop derived with Solar TErrestrial RElations Observatory/EUV Imager indicates that the strong redshift in the loop-top region is due to upflowing plasma originating from the jet. Both hard X-ray and soft X-ray emission from the Reuven Ramaty High Energy Solar Spectroscopic Imager were only seen as footpoint brightenings during the impulsive phase of the flare, then, soft X-ray emission moved to the loop top in the decay phase. Based on the temperature and density measurements and theoretical cooling models, the temperature evolution of the flare arch is consistent with impulsive heating during the jet eruption followed by conductive cooling via evaporation and minor prolonged heating in the top of the fan loop. Investigating the magnetic field topology and squashing factor map from Solar Dynamics Observatory/HMI, we conclude that the observed magnetic-fan flaring arch is mostly heated from low atmospheric reconnection accompanying the jet ejection, instead of from reconnection above the arch as expected in the standard flare model. Title: Possible Production of Solar Spicules by Microfilament Eruptions Authors: Sterling, Alphonse C.; Moore, Ronald L.; Samanta, Tanmoy; Yurchyshyn, Vasyl Bibcode: 2020ApJ...893L..45S Altcode: 2020arXiv200404187S We examine Big Bear Solar Observatory (BBSO) Goode Solar Telescope (GST) high spatial resolution (0"06), high-cadence (3.45 s), Hα-0.8 Å images of central-disk solar spicules, using data of Samanta et al. We compare with coronal-jet chromospheric-component observations of Sterling et al. Morphologically, bursts of spicules, referred to as "enhanced spicular activities" by Samanta et al., appear as scaled-down versions of the jet's chromospheric component. Both the jet and the enhanced spicular activities appear as chromospheric-material strands, undergoing twisting-type motions of ∼20-50 km s-1 in the jet and ∼20-30 km s-1 in the enhanced spicular activities. Presumably, the jet resulted from a minifilament-carrying magnetic eruption. For two enhanced spicular activities that we examine in detail, we find tentative candidates for corresponding erupting microfilaments, but not the expected corresponding base brightenings. Nonetheless, the enhanced-spicular-activities' interacting mixed-polarity base fields, frequent-apparent-twisting motions, and morphological similarities to the coronal jet's chromospheric-temperature component, suggest that erupting microfilaments might drive the enhanced spicular activities but be hard to detect, perhaps due to Hα opacity. Degrading the BBSO/GST-image resolution with a 1"0-FWHM smoothing function yields enhanced spicular activities resembling the "classical spicules" described by, e.g., Beckers. Thus, a microfilament eruption might be the fundamental driver of many spicules, just as a minifilament eruption is the fundamental driver of many coronal jets. Similarly, a 0"5-FWHM smoothing renders some enhanced spicular activities to resemble previously reported "twinned" spicules, while the full-resolution features might account for spicules sometimes appearing as 2D-sheet-like structures. Title: CESM-release-cesm2.1.2 Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier; Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large; Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson; Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, Van; Vertenstein; Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner; Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand Bibcode: 2020zndo...3895328D Altcode: The Community Earth System Model release version cesm2.1.2 Title: Design and performance of the first IceAct demonstrator at the South Pole Authors: Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alispach, C.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Axani, S.; Backes, P.; Bagherpour, H.; Bai, X.; Balagopal V., A.; Barbano, A.; Bartos, I.; Barwick, S. W.; Bastian, B.; Baum, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K. -H.; Becker Tjus, J.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bohm, C.; Bohmer, M.; Börner, M.; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.; Bretz, T.; Bron, S.; Brostean-Kaiser, J.; Burgman, A.; Buscher, J.; Busse, R. S.; Carver, T.; Chen, C.; Cheung, E.; Chirkin, D.; Choi, S.; Clark, K.; Classen, L.; Coleman, A.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dave, P.; De Clercq, C.; DeLaunay, J. J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Diaz, A.; Díaz-Vélez, J. C.; Dujmovic, H.; Dunkman, M.; DuVernois, M. A.; Dvorak, E.; Eberhardt, B.; Ehrhardt, T.; Eller, P.; Engel, R.; Evans, J. J.; Evenson, P. A.; Fahey, S.; Farrag, K.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Fox, D.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garrappa, S.; Gartner, A.; Gerhardt, L.; Gernhaeuser, R.; Ghorbani, K.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Griffith, Z.; Griswold, S.; Günder, M.; Gündüz, M.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Hanson, K.; Haugen, J.; Haungs, A.; Hebecker, D.; Heereman, D.; Heix, P.; Helbing, K.; Hellauer, R.; Henningsen, F.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, B.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Holzapfel, K.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Huege, T.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.; Jonske, F.; Joppe, R.; Kalekin, O.; Kang, D.; Kang, W.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katori, T.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krauss, C. B.; Krings, K.; Krückl, G.; Kulacz, N.; Kurahashi, N.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lazar, J. P.; Leonard, K.; Leszczyńska, A.; Leuermann, M.; Liu, Q. R.; Lohfink, E.; LoSecco, J.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Lünemann, J.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Makino, Y.; Mallik, P.; Mallot, K.; Mancina, S.; Mandalia, S.; Mariş, I. C.; Marka, S.; Marka, Z.; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Medina, A.; Meier, M.; Meighen-Berger, S.; Menne, T.; Merino, G.; Meures, T.; Micallef, J.; Mockler, D.; Momenté, G.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, M.; Muth, P.; Nagai, R.; Nakarmi, P.; Naumann, U.; Neer, G.; Niederhausen, H.; Nisa, M. U.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Oehler, M.; Olivas, A.; O'Murchadha, A.; O'Sullivan, E.; Palczewski, T.; Pandya, H.; Pankova, D. V.; Papp, L.; Park, N.; Peiffer, P.; Pérez de los Heros, C.; Petersen, T. C.; Philippen, S.; Pieloth, D.; Pinat, E.; Pinfold, J. L.; Pizzuto, A.; Plum, M.; Porcelli, A.; Price, P. B.; Przybylski, G. T.; Raab, C.; Rädel, L.; Raissi, A.; Rameez, M.; Rauch, L.; Rawlins, K.; Rea, I. C.; Reimann, R.; Relethford, B.; Renschler, M.; Renzi, G.; Resconi, E.; Rhode, W.; Richman, M.; Riegel, M.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Safa, I.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Sandstrom, P.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Schaufel, M.; Schieler, H.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schoenen, S.; Schröder, F. G.; Schumacher, J.; Schumacher, L.; Sclafani, S.; Seckel, D.; Seunarine, S.; Shaevitz, M. H.; Shefali, S.; Silva, M.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Söldner-Rembold, S.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Steinmüller, P.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strotjohann, N. L.; Stürwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Taketa, A.; Tanaka, H. K. M.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tilav, S.; Tollefson, K.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Ty, B.; Unger, E.; Unland Elorrieta, M. A.; Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijk, D.; van Eijndhoven, N.; Vanheule, S.; van Santen, J.; Veberic, D.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Watson, T. B.; Weaver, C.; Weindl, A.; Weiss, M. J.; Weldert, J.; Wendt, C.; Werthebach, J.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woschnagg, K.; Wrede, G.; Wren, S.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Yuan, T.; Zöcklein, M. Bibcode: 2020JInst..15.2002A Altcode: 2019arXiv191006945A In this paper we describe the first results of IceAct, a compact imaging air-Cherenkov telescope operating in coincidence with the IceCube Neutrino Observatory (IceCube) at the geographic South Pole. An array of IceAct telescopes (referred to as the IceAct project) is under consideration as part of the IceCube-Gen2 extension to IceCube. Surface detectors in general will be a powerful tool in IceCube-Gen2 for distinguishing astrophysical neutrinos from the dominant backgrounds of cosmic-ray induced atmospheric muons and neutrinos: the IceTop array is already in place as part of IceCube, but has a high energy threshold. Although the duty cycle will be lower for the IceAct telescopes than the present IceTop tanks, the IceAct telescopes may prove to be more effective at lowering the detection threshold for air showers. Additionally, small imaging air-Cherenkov telescopes in combination with IceTop, the deep IceCube detector or other future detector systems might improve measurements of the composition of the cosmic ray energy spectrum. In this paper we present measurements of a first 7-pixel imaging air Cherenkov telescope demonstrator, proving the capability of this technology to measure air showers at the South Pole in coincidence with IceTop and the deep IceCube detector. Title: Hi-C 2.1 Observations of Small-scale Miniature-filament-eruption-like Cool Ejections in an Active Region Plage Authors: Sterling, Alphonse C.; Moore, Ronald L.; Panesar, Navdeep K.; Reardon, Kevin P.; Molnar, Momchil; Rachmeler, Laurel A.; Savage, Sabrina L.; Winebarger, Amy R. Bibcode: 2020ApJ...889..187S Altcode: 2019arXiv191202319S We examine 172 Å ultra-high-resolution images of a solar plage region from the High-Resolution Coronal Imager, version 2.1 (Hi-C 2.1, or Hi-C) rocket flight of 2018 May 29. Over its five minute flight, Hi-C resolved a plethora of small-scale dynamic features that appear near noise level in concurrent Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) 171 Å images. For 10 selected events, comparisons with AIA images at other wavelengths and with Interface Region Imaging Spectrograph (IRIS) images indicate that these features are cool (compared to the corona) ejections. Combining Hi-C 172 Å, AIA 171 Å, IRIS 1400 Å, and Hα, we see that these 10 cool ejections are similar to the Hα "dynamic fibrils" and Ca II "anemone jets" found in earlier studies. The front of some of our cool ejections are likely heated, showing emission in IRIS 1400 Å. On average, these cool ejections have approximate widths 3"2 ± 2"1, (projected) maximum heights and velocities 4"3 ± 2"5 and 23 ± 6 km s-1, and lifetimes 6.5 ± 2.4 min. We consider whether these Hi-C features might result from eruptions of sub-minifilaments (smaller than the minifilaments that erupt to produce coronal jets). Comparisons with SDO's Helioseismic and Magnetic Imager (HMI) magnetograms do not show magnetic mixed-polarity neutral lines at these events' bases, as would be expected for true scaled-down versions of solar filaments/minifilaments. But the features' bases are all close to single-polarity strong-flux-edge locations, suggesting possible local opposite-polarity flux unresolved by HMI. Or it may be that our Hi-C ejections instead operate via the shock-wave mechanism that is suggested to drive dynamic fibrils and the so-called type I spicules. Title: Improving the Forecasting of Drivers of Severe Space Weather with the New MAG4 HMI Vector Magnetogram Database Authors: Fisher, M. A.; Falconer, D.; Moore, R.; Tiwari, S. Bibcode: 2020AAS...23521001F Altcode: MAG4 (MAGnetogram FOREcasting) is a large-database space-weather forecasting tool that makes near-real-time forecasts of a solar active regions (AR's) next-day chance of producing major eruptions (e.g., major flares or major Coronal Mass Ejections [CMEs]) that can drive severe space weather. The centerpiece of MAG4 is a pair of AR-event-rate forecasting curves obtained from a large database of (1) AR major-eruption histories and (2) an AR free-magnetic-energy proxy computed from magnetograms of the ARs. The pair of curves currently used for forecasting major flares are from MAG4's large database built from Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) AR line-of-sight (LOS) magnetograms and major-flare histories. Because MDI is now defunct, to forecast a current AR's major-flare rate, MAG4 presently uses the vertical-field component of the AR's Solar Dynamics Observatory (SDO)/ Helioseismic and Magnetic Imager (HMI) vector magnetogram to approximate the AR's MDI LOS magnetogram. Now that MAG4 has compiled a new comparably large database of AR major-flare histories and several alternative AR free-energy proxies computed from HMI vector magnetograms, we can quantify the improvement in MAG4's AR major-flare forecasts resulting from using the AR's HMI vector magnetogram with the pair of forecasting curves from MAG4's new HMI database instead of the presently-used pair from MAG4's MDI database. Using the Heidke Skill Score (HSS) and the statistical methods of Falconer et al. (2014), we show that this change gives for an optimized free-energy proxy (1) gives a 10-σ improvement in MAG4's major-flare forecasting performance, and (2) forecasting performance that ties or significantly exceeds that of the alternative AR free-energy proxies that are in the new database. Title: A CME-Producing Solar Eruption from the Interior of a Twisted Emerging Bipole Authors: Moore, R. L.; Adams, M.; Panesar, N. K.; Falconer, D. A.; Tiwari, S. K. Bibcode: 2019AGUFMSH43D3355M Altcode: In a negative-polarity coronal hole, magnetic flux emergence, seen by the Solar Dynamics Observatory's (SDO) Helioseismic Magnetic Imager (HMI), begins at approximately 19:00 UT on March 3, 2016. The emerged magnetic field produced sunspots with penumbrae by 3:00 UT on March 4, which NOAA numbered 12514. The emerging magnetic field is largely bipolar with the opposite-polarity fluxes spreading apart overall, but there is simultaneously some convergence and cancellation of opposite-polarity flux at the polarity inversion line (PIL) inside the emerging bipole. The emerging bipole shows obvious overall left-handed shear and/or twist in its magnetic field and corresponding clockwise rotation of the two poles of the bipole about each other as the bipole emerges. The eruption comes from inside the emerging bipole and blows it open to produce a CME observed by SOHO/LASCO. That eruption is preceded by flux cancellation at the emerging bipole's interior PIL, cancellation that plausibly builds a sheared and twisted flux rope above the interior PIL and finally triggers the blow-out eruption of the flux rope via photospheric-convection-driven slow tether-cutting reconnection of the legs of the sheared core field, low above the interior PIL, as proposed by van Ballegooijen and Martens (1989, ApJ, 343, 971) and Moore and Roumeliotis (1992, in Eruptive Solar Flares, ed. Z. Svestka, B.V. Jackson, and M.E. Machado [Berlin:Springer], 69). The production of this eruption is a (perhaps rare) counterexample to solar eruptions that result from external collisional shearing between opposite polarities from two distinct emerging and/or emerged bipoles (Chintzoglou et al., 2019, ApJ, 871:67). Title: A Two-Sided-Loop X-Ray Solar Coronal Jet and a Sudden Photospheric Magnetic-field Change, Both Driven by a Minifilament Eruption Authors: Sterling, A. C.; Harra, L. K.; Moore, R. L.; Falconer, D. A. Bibcode: 2019AGUFMSH11D3382S Altcode: Most of the commonly discussed solar coronal jets are of the type consisting of a
single spire extending approximately vertically from near the solar surface into the corona. Recent research shows that eruption of a miniature filament (minifilament) drives at least many such single-spire jets, and concurrently generates a miniflare at the eruption site. A different type of coronal jet, identified in X-ray images during the Yohkoh era, are two-sided-loop jets, which extend from a central excitation location in opposite directions, along two opposite low-lying coronal loops that are more-or-less horizontal to the surface. We observe such a two-sided-loop jet from the edge of active region (AR) 12473, using data from Hinode XRT and EIS, and SDO AIA and HMI. Similar to single-spire jets, this two-sided-loop jet results from eruption of a minifilament, which accelerates to over 140 km/s before abruptly stopping upon striking overlying nearly-horizontal magnetic field at ∼ 30,000 km altitude and producing the two-sided-loop jet via interchange reconnection. Analysis of EIS raster scans show that a hot brightening, consistent with a small flare, develops in the aftermath of the eruption, and that Doppler motions (∼ 40 km/s) occur near the jet-formation region. As with many single-spire jets, the trigger of the eruption here is apparently magnetic flux cancelation, which occurs at a rate of ∼ 4×10^18 Mx/hr, comparable to the rate observed in some single-spire AR jets. An apparent increase in the (line-of-sight) flux occurs within minutes of onset of the minifilament eruption, consistent with the apparent increase being due to a rapid reconfiguration of low-lying magnetic field during the minifilament eruption. Details appear in Sterling et al. (2019, ApJ, 871, 220). Title: Are the brightest coronal loops always rooted in mixed-polarity magnetic flux? Authors: Evans, C.; Tiwari, S. K.; Panesar, N. K.; Prasad, A.; Moore, R. L. Bibcode: 2019AGUFMSH41F3324E Altcode: Magnetic energy dissipated in coronal loops heats the Sun's corona to millions of Kelvin. Some recent investigations indicate that in addition to the required magnetoconvection and field strength, heating in the brightest coronal loops are driven by flux cancellation at the loop-feet. To find coronal loop footpoints , we selected extreme ultraviolet (EUV) data from the Atmospheric Imaging Assembly (AIA) and line- of-sight (LOS) magnetograms from the Helioseismic and Magnetic Imager (HMI), both on-board the Solar Dynamics Observatory (SDO). We located the footpoints of 28 brightest coronal loops of the bipolar active region NOAA 12712 on 28 May 2018 in hot 94 images (calculated using the Warren et al. method) and confirm the location of these footpoints via non-force free field extrapolations. We examine the photospheric magnetic field in 6" boxes centered at each footpoint and find that ~20% of loops have both feet in unipolar magnetic flux, ~10% loops have both feet in mixed-polarity flux, and ~70% of loops have one foot in unipolar and one in mixed-polarity flux. The presence of mixed-polarity magnetic flux in at least one foot of majority of the brightest coronal loops suggests that flux cancellation at the footpoints may drive heating in them. However, the absence of mixed-polarity magnetic flux (to the detection limit of HMI) in a significant number of the brightest coronal loops suggests that flux cancellation may not be necessary to drive heating in the loops - the combination of magnetoconvection and the magnetic field strength at the footpoints could be responsible for much of the coronal loop heating even in cases where a footpoint presents mixed-polarity magnetic flux. Title: Hi-C 2.1 Observations of Jetlet-like Events at Edges of Solar Magnetic Network Lanes Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L.; Winebarger, Amy R.; Tiwari, Sanjiv K.; Savage, Sabrina L.; Golub, Leon E.; Rachmeler, Laurel A.; Kobayashi, Ken; Brooks, David H.; Cirtain, Jonathan W.; De Pontieu, Bart; McKenzie, David E.; Morton, Richard J.; Peter, Hardi; Testa, Paola; Walsh, Robert W.; Warren, Harry P. Bibcode: 2019ApJ...887L...8P Altcode: 2019arXiv191102331P We present high-resolution, high-cadence observations of six, fine-scale, on-disk jet-like events observed by the High-resolution Coronal Imager 2.1 (Hi-C 2.1) during its sounding-rocket flight. We combine the Hi-C 2.1 images with images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and the Interface Region Imaging Spectrograph (IRIS), and investigate each event’s magnetic setting with co-aligned line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). We find that (i) all six events are jetlet-like (having apparent properties of jetlets), (ii) all six are rooted at edges of magnetic network lanes, (iii) four of the jetlet-like events stem from sites of flux cancelation between majority-polarity network flux and merging minority-polarity flux, and (iv) four of the jetlet-like events show brightenings at their bases reminiscent of the base brightenings in coronal jets. The average spire length of the six jetlet-like events (9000 ± 3000 km) is three times shorter than that for IRIS jetlets (27,000 ± 8000 km). While not ruling out other generation mechanisms, the observations suggest that at least four of these events may be miniature versions of both larger-scale coronal jets that are driven by minifilament eruptions and still-larger-scale solar eruptions that are driven by filament eruptions. Therefore, we propose that our Hi-C events are driven by the eruption of a tiny sheared-field flux rope, and that the flux rope field is built and triggered to erupt by flux cancelation. Title: Fine-scale explosive energy release at sites of magnetic flux cancellation in the core of the solar active region observed by Hi-C 2.1, IRIS and SDO Authors: Tiwari, S. K.; Panesar, N. K.; Moore, R. L.; De Pontieu, B.; Winebarger, A. R. Bibcode: 2019AGUFMSH31C3323T Altcode: The second sounding-rocket flight of the High-Resolution Coronal Imager (Hi-C 2.1) provided unprecedentedly-high spatial and temporal resolution Title: CME-Forecasting Performance of MAG4 with its HMI Vector Magnetogram Database Authors: Schragal, N. T.; Falconer, D. A.; Tiwari, S. K.; Moore, R. L. Bibcode: 2019AGUFMSH33C3354S Altcode: Coronal mass ejections (CMEs), solar flares, and solar proton events (SPEs) pose a threat to space-based infrastructure and astronauts. Many years of developmental work on predicting these events from active region (AR) magnetograms from MDI and HMI have led to MAG4 (MAGnetogram FOREcasting), a large-database forecasting technique for near-real-time forecasting of the next-day major flare, CME, and SPE productivity of an AR. MAG4 uses a free-magnetic-energy proxy computed for the AR from an HMI magnetogram and the AR's previous-day major-flare productivity in conjunction with a pair of forecasting curves derived from MAG4's large database of AR magnetograms to forecast these events. Previous work on improving the major-flare forecasting performance of MAG4 by deriving the forecasting curves from HMI vector magnetograms instead of from MDI line-of-sight magnetograms has laid the groundwork for improving the CME and SPE forecasting of MAG4. The present work is a first step in similarly improving MAG4's CME forecasting performance. We use MAG4's HMI AR vector magnetograms and a list of AR-produced CME events during August 2010 - March 2014. As done previously for major flares, we carry out 3000 random divisions of the observed set of ARs into a control half-set and an experimental half-set to determine the forecasting performance of each of 48 different parameters computed from the AR magnetograms. Each control set gives the pair of CME forecasting curves for each parameter. Then these curves are used to forecast the next-day event rate from each AR magnetogram in the experimental set. We measure forecasting performance by the Heidke Skill score which ranges from -∞ to 1, where a score of 0 is for performance that is no better than random chance, negative scores are for performance worse than random chance, and 1 is for perfect performance. Preliminary results indicate that the best-performing AR magnetogram parameters for predicting CMEs are not the same as the ones for major flares. Title: Cradle-to-Grave Evolution and Explosiveness of the Magnetic Field from Bipolar Ephemeral Active Regions (BEARs) in Solar Coronal Holes Authors: Panesar, N. K.; Nagib, C.; Moore, R. L.; Sterling, A. C. Bibcode: 2019AGUFMSH11D3386P Altcode: We report on the entire magnetic evolution and history of magnetic-explosion eruption production of each of 7 bipolar ephemeral active regions (BEARs) observed in on-disk coronal holes in line-of-sight magnetograms and in coronal EUV images. One of these BEARs made no eruptions. The other 6 BEARs together display three kinds of magnetic-explosion eruptions: (1) blowout eruptions (eruptions that make a wide-spire blowout jet), (2) partially-confined eruptions (eruptions that make a narrow-spire standard jet), (3) confined eruptions (eruptions that make no jet, i.e., make only a spireless EUV microflare). The 7 BEARs are a subset of a set of 60 random coronal-hole BEARs that were observed from the advent to the final dissolution of the BEAR's minority-polarity magnetic flux. The emergence phase (time interval from advent to maximum minority flux) for the 60 BEARs had been previously visually estimated using the magnetograms, to find if magnetic-explosion eruption events commonly occur inside a BEAR's emerging magnetic field (as had been assumed by Moore et al 2010, ApJ 720:757). That inspection found no inside eruption during the estimated emergence phase of any of the 60 BEARs. In this new work, for each of the 7 BEARs, we obtain a more reliable determination of when the emergence phase ended by finding the time of the BEAR's maximum minority flux from a time plot of the BEAR's minority flux measured from the magnetograms. These plots show: (1) none of the 7 BEARs had an inside eruption while the BEAR was emerging, and (2) for these 7 BEARs, the visually-estimated emergence end time was never more than 6 hours before the measured time of maximum minority flux. Of the 60 BEARs, in only 6 was there an inside eruption within 6 hours after the visually-estimated end of emergence. The above two results for the 7 BEARs, together with the previous visual inspection of the 60 BEARs, support that a great majority (at least 90%) of the explosive magnetic fields from BEARs in coronal holes are prepared and triggered to explode by magnetic flux cancellation, and that such flux cancellation seldom occurs inside an emerging BEAR. The visual inspection of the magnetograms of the 60 BEARs showed that the pre-eruption flux cancellation was either on the outside of the BEAR during or after the BEAR's emergence or on the inside of the BEAR after the BEAR's emergence. Title: Onset of the Magnetic Explosion in On-disk Solar Coronal Jets Authors: Panesar, N. K.; Moore, R. L.; Sterling, A. C. Bibcode: 2019AGUFMSH11D3384P Altcode: In our recent studies of ~10 quiet region and ~13 coronal hole coronal, we found that flux cancelation is the fundamental process in the buildup and triggering of the minifilament eruption that drives the production of the jet. Here, we investigate the onset and growth of the ten on-disk quiet region jets, using EUV images from SDO/AIA and magnetograms from SDO/HMI. We find that: (i) in all ten events the minifilament starts to rise at or before the onset of the signature of internal or external reconnection; (ii) in two out of ten jets brightening from the external reconnection starts at the same time as the slow rise of the minifilament and (iii) in six out of ten jets brightening from the internal reconnection starts before the start of the brightening from external reconnection. These observations show that the magnetic explosion in coronal jets begins in the same way as the magnetic explosion in filament eruptions that make solar flares and coronal mass ejections (CMEs). Our results indicate (1) that coronal jets are miniature versions of CME-producing eruptions and flux cancelation is the fundamental process that builds and triggers both the small-scale and the large-scale eruptions, and (2) that, contrary to the view of Moore et al (2018), the current sheet at which the external reconnection occurs in coronal jets usually starts to form at or after the onset of (and as a result of) the slow rise of the minifilament flux-rope eruption, and so is seldom of appreciable size before the onset of the slow rise of the minifilament flux-rope eruption. Title: Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO Authors: Tiwari, Sanjiv K.; Panesar, Navdeep K.; Moore, Ronald L.; De Pontieu, Bart; Winebarger, Amy R.; Golub, Leon; Savage, Sabrina L.; Rachmeler, Laurel A.; Kobayashi, Ken; Testa, Paola; Warren, Harry P.; Brooks, David H.; Cirtain, Jonathan W.; McKenzie, David E.; Morton, Richard J.; Peter, Hardi; Walsh, Robert W. Bibcode: 2019ApJ...887...56T Altcode: 2019arXiv191101424T The second Hi-C flight (Hi-C 2.1) provided unprecedentedly high spatial and temporal resolution (∼250 km, 4.4 s) coronal EUV images of Fe IX/X emission at 172 Å of AR 12712 on 2018 May 29, during 18:56:21-19:01:56 UT. Three morphologically different types (I: dot-like; II: loop-like; III: surge/jet-like) of fine-scale sudden-brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. Although type Is (not reported before) resemble IRIS bombs (in size, and brightness with respect to surroundings), our dot-like events are apparently much hotter and shorter in span (70 s). We complement the 5 minute duration Hi-C 2.1 data with SDO/HMI magnetograms, SDO/AIA EUV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying likely flux cancellation at the microflare’s polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. In types I and II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow. The light curves from Hi-C, AIA, and IRIS peak nearly simultaneously for many of these events, and none of the events display a systematic cooling sequence as seen in typical coronal flares, suggesting that these tiny brightening events have chromospheric/transition region origin. Title: Further Evidence for Magnetic Flux Cancelation as the Build-up and Trigger Mechanism for Eruptions in Isolated Solar Active Regions Authors: Sterling, A. C.; Buell, A.; Moore, R. L.; Falconer, D. A. Bibcode: 2019AGUFMSH11D3388S Altcode: We examine the magnetic evolution of three eruption-producing solar active regions (ARs), one each from 2013, 2014, and 2017, using data from SDO HMI and AIA. Each of the ARs is relatively small, so that we can follow its entire development during a single disk passage, from birth by emergence through the time of the respective eruptions; the first-, second-, and third-born respectively lived 3, 6.5, and 3 days before eruption. Each AR was relatively isolated, with minimal interaction with surrounding ARs, allowing us to study each AR as an approximately isolated system. CMEs resulted from eruptions in the first two ARs, while the third AR's eruption was smaller and appeared confined. In each AR, the eruption was seated on an interval of the AR's magnetic polarity inversion line (neutral line) where opposite-polarity flux was merging together and undergoing apparent cancelation. Our results, together with an earlier pilot study of two ARs by Sterling et al. (2018), and along with recent studies of solar coronal jets, support the view that the magnetic field that explodes to produce solar eruptions of size scales ranging from jets to CMEs are usually built and triggered by flux cancelation along a sharp neutral line. Title: Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets Authors: McGlasson, Riley A.; Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2019ApJ...882...16M Altcode: 2019arXiv190606452M Coronal jets are transient narrow features in the solar corona that originate from all regions of the solar disk: active regions, quiet Sun, and coronal holes. Recent studies indicate that at least some coronal jets in quiet regions and coronal holes are driven by the eruption of a minifilament following flux cancellation at a magnetic neutral line. We have tested the veracity of that view by examining 60 random jets in quiet regions and coronal holes using multithermal (304, 171, 193, and 211 Å) extreme ultraviolet images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly and line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager. By examining the structure and changes in the magnetic field before, during, and after jet onset, we found that 85% of these jets resulted from a minifilament eruption triggered by flux cancellation at the neutral line. The 60 jets have a mean base diameter of 8800 ± 3100 km and a mean duration of 9 ± 3.6 minutes. These observations confirm that minifilament eruption is the driver and magnetic flux cancellation is the primary trigger mechanism for most coronal hole and quiet region coronal jets. Title: CESM-release-cesm2.1.1 Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier; Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large; Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson; Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, van; Vertenstein; Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner; Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand Bibcode: 2019zndo...3895315D Altcode: The Community Climate Earth System Model release version cesm2.1.1 Title: Understanding the Mechanisms of Sulfate Formation in Acidic Volcanic Hydrothermal Environments on Mars Using Terrestrial Analogs Authors: Ende, J. J.; Faiia, A. M.; Burtt, P.; Moore, R.; Szynkiewicz, A. Bibcode: 2019LPICo2089.6212E Altcode: In this study, we use a combination of chemistry and oxygen isotopes as tracers for the oxidation mechanism of sulfate in volcanic acidic hydrothermal systems on Earth to better understand how sulfate forms in similar environments on Mars. Title: Fine-scale explosive energy release at sites of magnetic flux cancellation in the core of the solar active region observed by HiC2.1, IRIS and SDO Authors: Tiwari, Sanjiv K.; Panesar, Navdeep; Moore, Ronald L.; De Pontieu, Bart; Testa, Paola; Winebarger, Amy R. Bibcode: 2019AAS...23411702T Altcode: The second sounding-rocket flight of the High-Resolution Coronal Imager (HiC2.1) provided unprecedentedly-high spatial and temporal resolution (150 km, 4.5 s) coronal EUV images of Fe IX/X emission at 172 Å, of a solar active region (AR NOAA 12712) near solar disk center. Three morphologically-different types (I: dot-like, II: loop-like, & III: surge/jet-like) of fine-scale sudden brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. We complement the 5-minute-duration HiC2.1 data with SDO/HMI magnetograms, SDO/AIA EUV and UV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying flux cancellation at the polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. These outflows from both ends of the arch filament system are seen as bi-directional flows in the arch filament system, suggesting that the well-known counter-streaming flows in large classical filaments could be driven in the same way as in this arch filament system: by fine-scale jet-like explosions from fine-scale sites of mixed-polarity field in the feet of the sheared field that threads the filament. Plausibly, the flux cancellation at these sites prepares and triggers a fine scale core-magnetic-field structure (a small sheared/twisted core field or flux rope along and above the cancellation line) to explode. In types I & II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow in the manner of larger jets in coronal holes, quiet regions, and active regions. Title: Hi-C2.1 Observations of Solar Jetlets at Sites of Flux Cancelation Authors: Panesar, Navdeep; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2019AAS...23411701P Altcode: Solar jets of all sizes are magnetically channeled narrow eruptive events; the larger ones are often observed in the solar corona in EUV and coronal X-ray images. Recent observations show that the buildup and triggering of the minifilament eruptions that drive coronal jets result from magnetic flux cancelation under the minifilament, at the neutral line between merging majority-polarity and minority-polarity magnetic flux patches. Here we investigate the magnetic setting of six on-disk small-scale jet-like/spicule-like eruptions (also known as jetlets) by using high resolution 172A images from the High-resolution Coronal Imager (Hi-C2.1) and EUV images from Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and line-of-sight magnetograms from SDO/Helioseismic and Magnetic Imager (HMI). From magnetograms co-aligned with the Hi-C and AIA images, we find that (i) these jetlets are rooted at edges of magnetic network lanes (ii) some jetlets stem from sites of flux cancelation between merging majority-polarity and minority-polarity flux patches (iii) some jetlets show faint brightenings at their bases reminiscent of the base brightenings in coronal jets. Based on the 6 Hi-C jetlets that we have examined in detail and our previous observations of 30 coronal jets in quiet regions and coronal holes, we infer that flux cancelation is the essential process in the buildup and triggering of jetlets. Our observations suggest that network jetlets result from small-scale eruptions that are analogs of both larger-scale coronal jet minifilament eruptions and the still-larger-scale eruptions that make major CMEs. This work was supported by the NASA/MSFC NPP program and the NASA HGI Program. Title: Invisibility of Solar Active Region Umbra-to-Umbra Coronal Loops: New Evidence that Magnetoconvection Drives Solar-Stellar Coronal Heating Authors: Moore, Ronald L.; Tiwari, Sanjiv; Thalmann, Julia; Panesar, Navdeep; Winebarger, Amy Bibcode: 2019AAS...23410603M Altcode: How magnetic energy is injected and released in the solar corona, keeping it heated to several million degrees, remains elusive. The corona is shaped by the magnetic field that fills it and the heating of the corona generally increases with increasing strength of the field. For each of two bipolar solar active regions having one or more sunspots in each of the two main opposite-polarity domains of magnetic flux, from comparison of a nonlinear force-free model of the active region's three-dimensional coronal magnetic field to observed extreme-ultraviolet coronal loops, we find that (1) umbra-to-umbra loops, despite being rooted in the strongest magnetic flux at both ends, are invisible, and (2) the brightest loops have one foot in a sunspot umbra or penumbra and the other foot in another sunspot's penumbra or in unipolar or mixed-polarity plage. The invisibility of umbra-to-umbra loops is new evidence that magnetoconvetion drives solar-stellar coronal heating: evidently, the strong umbral field at both ends quenches the magnetoconvection and hence the heating. Broadly, our results indicate that depending on the field strength in both feet, the photospheric feet of a coronal loop on any convective star can either engender or quench coronal heating in the body of the loop. This work was supported by funding from the Heliophysics Division of NASA's Science Mission Directorate, from NASA's Postdoctoral Program, and from the Austrian Science Fund. The results have been published in The Astrophysical Journal Letters (Tiwari, S. K., Thalmann, J. K., Panesar, N. K., Moore, R. L., & Winebarger, A. R. 2017, ApJ Letters, 843:L20). Title: A CME-Producing Solar Eruption from the Interior of an Emerging Bipolar Active Region Authors: Adams, Mitzi L.; Moore, Ronald L.; Panesar, Navdeep; Falconer, David Bibcode: 2019AAS...23430501A Altcode: In a negative-polarity coronal hole, magnetic flux emergence, seen by the Solar Dynamics Observatory's (SDO) Helioseismic Magnetic Imager (HMI), begins at approximately 19:00 UT on March 3, 2016. The emerged magnetic field produced sunspots, which NOAA numbered 12514 two days later. The emerging magnetic field is largely bipolar with the opposite-polarity fluxes spreading apart overall, but there is simultaneously some convergence and cancellation of opposite-polarity flux at the polarity inversion line (PIL) inside the emerging bipole. In the first fifteen hours after emergence onset, three obvious eruptions occur, observed in the coronal EUV images from SDO's Atmospheric Imaging Assembly (AIA). The first two erupt from separate segments of the external PIL between the emerging positve-polarity flux and the extant surrounding negative-polarity flux, with the exploding magnetic field being prepared and triggered by flux cancellation at the external PIL. The emerging bipole shows obvious overall left-handed shear and/or twist in its magnetic field. The third and largest eruption comes from inside the emerging bipole and blows it open to produce a CME observed by SOHO/LASCO. That eruption is preceded by flux cancellation at the emerging bipole's interior PIL, cancellation that plausibly builds a sheared and twisted flux rope above the interior PIL and finally triggers the blow-out eruption of the flux rope via photospheric-convection-driven slow tether-cutting reconnection of the legs of the sheared core field, low above the interior PIL, as proposed by van Ballegooijen and Martens (1989, ApJ, 343, 971) and Moore and Roumeliotis (1992, in Eruptive Solar Flares, ed. Z. Svestka, B.V. Jackson, and M.E. Machado [Berlin:Springer], 69). The production of this eruption is a (perhaps rare) counterexample to solar eruptions that result from external collisional shearing between opposite polarities from two distinct emerging and/or emerged bipoles (Chintzoglou et al., 2019, ApJ, 871:67). This work was supported by NASA, the NASA Postdoctoral Program (NPP), and NSF. Title: Incorporating Students into Investigations of the Effects of Solar Eclipse Totality on Biological Organisms Authors: Sudbrink, D. L., Jr.; Mills, R.; Moore, R.; Rendleman, E. Bibcode: 2019ASPC..516..457S Altcode: Environmental changes during total solar eclipses can have impacts on behaviors of biological organisms. Observations of behaviors of several species of organisms were conducted during the Great American Eclipse of 21 August 2017 in Tennessee with students from U.S. Space & Rocket Center Space Camp, Project INSPIRE and Austin Peay State University. Detailed observations were made of crickets, honeybees, cattle and turtles during this study. Results indicated that there were at least temporary alterations of typical diurnal behavior of many of the animals studied near or during the totality of the eclipse. In these instances, typical diurnal behaviors were observed to resume after totality. Title: Improving Forecasting of Drivers of Severe Space Weather with the New MAG4 HMI Vector Magnetogram Database Authors: Falconer, David; Tiwari, Sanjiv; Moore, Ronald; Fisher, Megan Bibcode: 2019AAS...23431705F Altcode: Major solar flares and Coronal Mass Ejections (CMEs) are drivers of severe space weather. The strongest ones come from active regions (ARs). They are powered by explosive release of magnetic energy. MAG4 (Magnetogram Forecast) is a large-database near-real-time tool that measures an AR's free-energy proxy from the AR's deprojected HMI vector magnetograms. MAG4 converts the free-energy proxy to the AR's predicted event rate (and event probability) using a forecasting curve. MAG4 forecasts the event rate and probability for each AR on the disk, as well as for the full disk. The forecasting curves presently used by MAG4 are derived from a large sample of SOHO/MDI AR magnetograms. This requires the HMI vector magnetograms to be degraded in spatial resolution to approximate what MDI would have measured, in order to use the MDI forecasting curves. We report on the improved performance of MAG4 that results from using forecasting curves based on MAG4's new database of HMI vector magnetograms instead of using the present forecasting curves that are based on MDI line-of-sight magnetograms. MAG4's forecasting skill score significantly improves for major flares (M1 or greater). We present MAG4's improvement in forecasting SPEs (Solar Particle Events) and X-class flares as well. The improvement in forecasting CMEs will be evaluated in the future. These new forecasting curves are being implemented in the near-real-time operational MAG4, though forecasts from the old curves will still be given. This work is funded by NSF's Solar Terrestrial Program, and NASA/SRAG. Title: A Two-Sided-Loop X-Ray Solar Coronal Jet and a Sudden Photospheric Magnetic-field Change, Both Driven by a Minifilament Eruption Authors: Sterling, Alphonse C.; Harra, Louise; Moore, Ronald L.; Falconer, David Bibcode: 2019AAS...23431701S Altcode: Most of the commonly discussed solar coronal jets are of the type consisting of a single spire extending approximately vertically from near the solar surface into the corona. Recent research shows that eruption of a miniature filament (minifilament) drives at least many such single-spire jets, and concurrently generates a miniflare at the eruption site. A different type of coronal jet, identified in X-ray images during the Yohkoh era, are two-sided-loop jets, which extend from a central excitation location in opposite directions, along two opposite low-lying coronal loops that are more-or-less horizontal to the surface. We observe such a two-sided-loop jet from the edge of active region (AR) 12473, using data from Hinode XRT and EIS, and SDO AIA and HMI. Similar to single-spire jets, this two-sided-loop jet results from eruption of a minifilament, which accelerates to over 140 km/s before abruptly stopping upon striking overlying nearly-horizontal magnetic field at ∼30,000 km altitude and producing the two-sided-loop jet via interchange reconnection. Analysis of EIS raster scans show that a hot brightening, consistent with a small flare, develops in the aftermath of the eruption, and that Doppler motions (∼40 km/s) occur near the jet-formation region. As with many single-spire jets, the trigger of the eruption here is apparently magnetic flux cancelation, which occurs at a rate of ∼4×1018 Mx/hr, comparable to the rate observed in some single-spire AR jets. An apparent increase in the (line-of-sight) flux occurs within minutes of onset of the minifilament eruption, consistent with the apparent increase being due to a rapid reconfiguration of low-lying magnetic field during the minifilament eruption. Details appear in Sterling et al. (2019, ApJ, 871, 220). Title: Sheared Magnetic Arcades and the Pre-eruptive Magnetic Configuration of Coronal Mass Ejections: Diagnostics, Challenges and Future Observables Authors: Patsourakos, Spiros; Vourlidas, A.; Anthiochos, S. K.; Archontis, V.; Aulanier, G.; Cheng, X.; Chintzoglou, G.; Georgoulis, M. K.; Green, L. M.; Kliem, B.; Leake, J.; Moore, R. L.; Nindos, A.; Syntelis, P.; Torok, T.; Yardley, S. L.; Yurchyshyn, V.; Zhang, J. Bibcode: 2019shin.confE.194P Altcode: Our thinking about the pre-eruptive magnetic configuration of Coronal Mass Ejections has been effectively dichotomized into two opposing and often fiercely contested views: namely, sheared magnetic arcades and magnetic flux ropes. Finding a solution to this issue will have important implications for our understanding of CME initiation. We first discuss the very value of embarking into the arcade vs. flux rope dilemma and illustrate the corresponding challenges and difficulties to address it. Next, we are compiling several observational diagnostics of pre-eruptive sheared magnetic arcades stemming from theory/modeling, discuss their merits, and highlight potential ambiguities that could arise in their interpretation. We finally conclude with a discussion of possible new observables, in the frame of upcoming or proposed instrumentation, that could help to circumvent the issues we are currently facing. Title: 2019 GA Authors: Ludwig, F.; Stecklum, B.; Tichy, M.; Ticha, J.; Baransky, A.; McCarthy Obs, J. J.; Robson, M.; Moore, R.; Cloutier, W.; Lindner, P.; Holmes, R.; Foglia, S.; Buzzi, L.; Linder, T.; Ye, Q. -Z.; Collaboration, Z. T. F.; Duev, D. A.; Lin, H. -W.; Mahabal, A. A.; Masci, F. J.; Streaks, D.; Groeller, H.; Kowalski, R. A.; Leonard, G. J.; Africano, B. M.; Christensen, E. J.; Farneth, G. A.; Fuls, D. C.; Gibbs, A. R.; Grauer, A. D.; Larson, S. M.; Pruyne, T. A.; Seaman, R. L.; Shelly, F. C.; Birtwhistle, P.; Favero, G.; Furgoni, R.; Adamovsky, M.; Korlevic, K.; Nishiyama, K.; Urakawa, S.; Flynn, R. L.; Wells, G.; Bamberger, D. Bibcode: 2019MPEC....G...29L Altcode: No abstract at ADS Title: A K-12 Microgravity Educational Intervention Framework Authors: Carmona, J. A.; Smith, S. L.; York, J.; Moore, R.; Clyat, M.; Buchs, T.; Laufer, R.; Attai, S.; Matthews, L. S.; Hyde, T. W. Bibcode: 2019LPI....50.1574C Altcode: The CASPER group has developed a STEM outreach program where participating students will have access to a 1.5s drop tower housed on the Baylor University campus. Title: A Two-sided Loop X-Ray Solar Coronal Jet Driven by a Minifilament Eruption Authors: Sterling, Alphonse C.; Harra, Louise K.; Moore, Ronald L.; Falconer, David A. Bibcode: 2019ApJ...871..220S Altcode: 2018arXiv181105557S Most of the commonly discussed solar coronal jets are the type that consist of a single spire extending approximately vertically from near the solar surface into the corona. Recent research supports that eruption of a miniature filament (minifilament) drives many such single-spire jets and concurrently generates a miniflare at the eruption site. A different type of coronal jet, identified in X-ray images during the Yohkoh era, are two-sided loop jets, which extend from a central excitation location in opposite directions, along low-lying coronal loops that are more-or-less horizontal to the surface. We observe such a two-sided loop jet from the edge of active region (AR) 12473, using data from Hinode X-Ray Telescope (XRT) and Extreme Ultraviolet Imaging Spectrometer (EIS), and from Solar Dynamics Observatory’s (SDO) Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI). Similar to single-spire jets, this two-sided loop jet results from eruption of a minifilament, which accelerates to over 140 km s-1 before abruptly stopping after striking an overlying nearly horizontal-loop field at ∼30,000 km in altitude and producing the two-sided loop jet. An analysis of EIS raster scans shows that a hot brightening, consistent with a small flare, develops in the aftermath of the eruption, and that Doppler motions (∼40 km s-1) occur near the jet formation region. As with many single-spire jets, the magnetic trigger here is apparently flux cancelation, which occurs at a rate of ∼4 × 1018 Mx hr-1, broadly similar to the rates observed in some single-spire quiet-Sun and AR jets. An apparent increase in the (line-of-sight) flux occurs within minutes of the onset of the minifilament eruption, consistent with the apparent increase being due to a rapid reconfiguration of low-lying fields during and soon after the minifilament-eruption onset. Title: All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field Authors: Abeysekara, A. U.; Alfaro, R.; Alvarez, C.; Arceo, R.; Arteaga-Velázquez, J. C.; Avila Rojas, D.; Belmont-Moreno, E.; BenZvi, S. Y.; Brisbois, C.; Capistrán, T.; Carramiana, A.; Casanova, S.; Cotti, U.; Cotzomi, J.; Díaz-Vélez, J. C.; De León, C.; De la Fuente, E.; Dichiara, S.; DuVernois, M. A.; Espinoza, C.; Fiorino, D. W.; Fleischhack, H.; Fraija, N.; Galván-Gámez, A.; García-González, J. A.; González, M. M.; Goodman, J. A.; Hampel-Arias, Z.; Harding, J. P.; Hernandez, S.; Hona, B.; Hueyotl-Zahuantitla, F.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Lara, A.; León Vargas, H.; Luis-Raya, G.; Malone, K.; Marinelli, S. S.; Martínez-Castro, J.; Martinez, O.; Matthews, J. A.; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Pérez-Pérez, E. G.; Pretz, J.; Ren, Z.; Rho, C. D.; Rivière, C.; Rosa-González, D.; Rosenberg, M.; Salazar, H.; Salesa Greus, F.; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Sinnis, G.; Smith, A. J.; Surajbali, P.; Taboada, I.; Tollefson, K.; Torres, I.; Villaseor, L.; Weisgarber, T.; Wood, J.; Zepeda, A.; Zhou, H.; Álvarez, J. D.; HAWC Collaboration; Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Argüelles, C.; Auffenberg, J.; Axani, S.; Backes, P.; Bagherpour, H.; Bai, X.; Barbano, A.; Barron, J. P.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Becker Tjus, J.; Becker, K. -H.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bohm, C.; Börner, M.; Bos, F.; Böser, S.; Botner, O.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.; Bretz, H. -P.; Bron, S.; Brostean-Kaiser, J.; Burgman, A.; Busse, R. S.; Carver, T.; Cheung, E.; Chirkin, D.; Clark, K.; Classen, L.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dave, P.; Day, M.; de André, J. P. A. M.; De Clercq, C.; DeLaunay, J. J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Díaz-Vélez, J. C.; Dujmovic, H.; Dunkman, M.; Dvorak, E.; Eberhardt, B.; Ehrhardt, T.; Eichmann, B.; Eller, P.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garrappa, S.; Gerhardt, L.; Ghorbani, K.; Giang, W.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Griffith, Z.; Haack, C.; Hallgren, A.; Halve, L.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.; Kalaczynski, P.; Kang, W.; Kappes, A.; Kappesser, D.; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, M.; Krückl, G.; Kunwar, S.; Kurahashi, N.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Leonard, K.; Leuermann, M.; Liu, Q. R.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lünemann, J.; Luszczak, W.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Makino, Y.; Mancina, S.; Mariş, I. C.; Maruyama, R.; Mase, K.; Maunu, R.; Meagher, K.; Medici, M.; Meier, M.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Micallef, J.; Momenté, G.; Montaruli, T.; Moore, R. W.; Moulai, M.; Nagai, R.; Nahnhauer, R.; Nakarmi, P.; Naumann, U.; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Olivas, A.; O'Murchadha, A.; O'Sullivan, E.; Palczewski, T.; Pandya, H.; Pankova, D. V.; Peiffer, P.; Pepper, J. A.; Pérez de los Heros, C.; Pieloth, D.; Pinat, E.; Pizzuto, A.; Plum, M.; Price, P. B.; Przybylski, G. T.; Raab, C.; Rameez, M.; Rauch, L.; Rawlins, K.; Rea, I. C.; Reimann, R.; Relethford, B.; Renzi, G.; Resconi, E.; Rhode, W.; Richman, M.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Safa, I.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Schaufel, M.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schöneberg, S.; Schumacher, L.; Sclafani, S.; Seckel, D.; Seunarine, S.; Soedingrekso, J.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strotjohann, N. L.; Stuttard, T.; Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tönnis, C.; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Ty, B.; Unger, E.; Unland Elorrieta, M. A.; Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijk, D.; van Eijndhoven, N.; Vanheule, S.; van Santen, J.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky, N.; Watson, T. B.; Weaver, C.; Weiss, M. J.; Wendt, C.; Werthebach, J.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woolsey, E.; Woschnagg, K.; Wrede, G.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Yuan, T.; IceCube Collaboration Bibcode: 2019ApJ...871...96A Altcode: 2018arXiv181205682H We present the first full-sky analysis of the cosmic ray arrival direction distribution with data collected by the High-Altitude Water Cherenkov and IceCube observatories in the northern and southern hemispheres at the same median primary particle energy of 10 TeV. The combined sky map and angular power spectrum largely eliminate biases that result from partial sky coverage and present a key to probe into the propagation properties of TeV cosmic rays through our local interstellar medium and the interaction between the interstellar and heliospheric magnetic fields. From the map, we determine the horizontal dipole components of the anisotropy δ 0h = 9.16 × 10-4 and δ 6h = 7.25 × 10-4 (±0.04 × 10-4). In addition, we infer the direction (229.°2 ± 3.°5 R.A., 11.°4 ± 3.°0 decl.) of the interstellar magnetic field from the boundary between large-scale excess and deficit regions from which we estimate the missing corresponding vertical dipole component of the large-scale anisotropy to be {δ }N∼ -{3.97}-2.0+1.0× {10}-4. Title: CESM-release-cesm2.1.0 Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier; Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large; Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson; Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, Van; Vertenstein; Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner; Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand Bibcode: 2018zndo...3895306D Altcode: The Community Earth System Model release version 2.1.0 Title: Evidence of Twisting and Mixed-polarity Solar Photospheric Magnetic Field in Large Penumbral Jets: IRIS and Hinode Observations Authors: Tiwari, Sanjiv K.; Moore, Ronald L.; De Pontieu, Bart; Tarbell, Theodore D.; Panesar, Navdeep K.; Winebarger, Amy R.; Sterling, Alphonse C. Bibcode: 2018ApJ...869..147T Altcode: 2018arXiv181109554T A recent study using Hinode (Solar Optical Telescope/Filtergraph [SOT/FG]) data of a sunspot revealed some unusually large penumbral jets that often repeatedly occurred at the same locations in the penumbra, namely, at the tail of a penumbral filament or where the tails of multiple penumbral filaments converged. These locations had obvious photospheric mixed-polarity magnetic flux in Na I 5896 Stokes-V images obtained with SOT/FG. Several other recent investigations have found that extreme-ultraviolet (EUV)/X-ray coronal jets in quiet-Sun regions (QRs), in coronal holes (CHs), and near active regions (ARs) have obvious mixed-polarity fluxes at their base, and that magnetic flux cancellation prepares and triggers a minifilament flux-rope eruption that drives the jet. Typical QR, CH, and AR coronal jets are up to 100 times bigger than large penumbral jets, and in EUV/X-ray images they show a clear twisting motion in their spires. Here, using Interface Region Imaging Spectrograph (IRIS) Mg II k λ2796 SJ images and spectra in the penumbrae of two sunspots, we characterize large penumbral jets. We find redshift and blueshift next to each other across several large penumbral jets, and we interpret these as untwisting of the magnetic field in the jet spire. Using Hinode/SOT (FG and SP) data, we also find mixed-polarity magnetic flux at the base of these jets. Because large penumbral jets have a mixed-polarity field at their base and have a twisting motion in their spires, they might be driven the same way as QR, CH, and AR coronal jets. Title: IRIS and SDO Observations of Solar Jetlets Resulting from Network-edge Flux Cancelation Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L.; Tiwari, Sanjiv K.; De Pontieu, Bart; Norton, Aimee A. Bibcode: 2018ApJ...868L..27P Altcode: 2018arXiv181104314P Recent observations show that the buildup and triggering of minifilament eruptions that drive coronal jets result from magnetic flux cancelation at the neutral line between merging majority- and minority-polarity magnetic flux patches. We investigate the magnetic setting of 10 on-disk small-scale UV/EUV jets (jetlets, smaller than coronal X-ray jets but larger than chromospheric spicules) in a coronal hole by using IRIS UV images and SDO/AIA EUV images and line-of-sight magnetograms from SDO/HMI. We observe recurring jetlets at the edges of magnetic network flux lanes in the coronal hole. From magnetograms coaligned with the IRIS and AIA images, we find, clearly visible in nine cases, that the jetlets stem from sites of flux cancelation proceeding at an average rate of ∼1.5 × 1018 Mx hr-1, and show brightenings at their bases reminiscent of the base brightenings in larger-scale coronal jets. We find that jetlets happen at many locations along the edges of network lanes (not limited to the base of plumes) with average lifetimes of 3 minutes and speeds of 70 km s-1. The average jetlet-base width (4000 km) is three to four times smaller than for coronal jets (∼18,000 km). Based on these observations of 10 obvious jetlets, and our previous observations of larger-scale coronal jets in quiet regions and coronal holes, we infer that flux cancelation is an essential process in the buildup and triggering of jetlets. Our observations suggest that network jetlet eruptions might be small-scale analogs of both larger-scale coronal jets and the still-larger-scale eruptions producing CMEs. Title: Magnetic Flux Cancelation as the Buildup and Trigger Mechanism for CME-producing Eruptions in Two Small Active Regions Authors: Sterling, Alphonse C.; Moore, Ronald L.; Panesar, Navdeep K. Bibcode: 2018ApJ...864...68S Altcode: 2018arXiv180703237S We follow two small, magnetically isolated coronal mass ejection (CME)-producing solar active regions (ARs) from the time of their emergence until several days later, when their core regions erupt to produce the CMEs. In both cases, magnetograms show: (a) following an initial period where the poles of the emerging regions separate from each other, the poles then reverse direction and start to retract inward; (b) during the retraction period, flux cancelation occurs along the main neutral line of the regions; (c) this cancelation builds the sheared core field/flux rope that eventually erupts to make the CME. In the two cases, respectively 30% and 50% of the maximum flux of the region cancels prior to the eruption. Recent studies indicate that solar coronal jets frequently result from small-scale filament eruptions, with those “minifilament” eruptions also being built up and triggered by cancelation of magnetic flux. Together, the small-AR eruptions here and the coronal jet results suggest that isolated bipolar regions tend to erupt when some threshold fraction, perhaps in the range of 50%, of the region's maximum flux has canceled. Our observed erupting filaments/flux ropes form at sites of flux cancelation, in agreement with previous observations. Thus, the recent finding that minifilaments that erupt to form jets also form via flux cancelation is further evidence that minifilaments are small-scale versions of the long-studied full-sized filaments. Title: Critical Magnetic Field Strengths for Solar Coronal Plumes in Quiet Regions and Coronal Holes? Authors: Avallone, Ellis A.; Tiwari, Sanjiv K.; Panesar, Navdeep K.; Moore, Ronald L.; Winebarger, Amy Bibcode: 2018ApJ...861..111A Altcode: 2018arXiv180511188A Coronal plumes are bright magnetic funnels found in quiet regions (QRs) and coronal holes (CHs). They extend high into the solar corona and last from hours to days. The heating processes of plumes involve dynamics of the magnetic field at their base, but the processes themselves remain mysterious. Recent observations suggest that plume heating is a consequence of magnetic flux cancellation and/or convergence at the plume base. These studies suggest that the base flux in plumes is of mixed polarity, either obvious or hidden in Solar Dynamics Observatory (SDO)/HMI data, but do not quantify it. To investigate the magnetic origins of plume heating, we select 10 unipolar network flux concentrations, four in CHs, four in QRs, and two that do not form a plume, and track plume luminosity in SDO/AIA 171 Å images along with the base flux in SDO/HMI magnetograms, over each flux concentration’s lifetime. We find that plume heating is triggered when convergence of the base flux surpasses a field strength of ∼200-600 G. The luminosity of both QR and CH plumes respond similarly to the field in the plume base, suggesting that the two have a common formation mechanism. Our examples of non-plume-forming flux concentrations, reaching field strengths of 200 G for a similar number of pixels as for a couple of our plumes, suggest that a critical field might be necessary to form a plume but is not sufficient for it, thus advocating for other mechanisms, e.g., flux cancellation due to hidden opposite-polarity field, at play. Title: Flux Cancelation as the Trigger of Coronal Hole Jet Eruptions Authors: Panesar, Navdeep Kaur; Sterling, Alphonse C.; Moore, Ronald Lee Bibcode: 2018tess.conf40806P Altcode: Coronal jets are magnetically channeled narrow eruptions often observed in the solar corona. Recent observations show that coronal jets are driven by the eruption of a small-scale filament (minifilament). Here we investigate the triggering mechanism of jet-driving minifilament eruptions in coronal holes, by using X-ray images from Hinode, EUV images from SDO/AIA, and line of sight magnetograms from SDO/HMI. We study 13 on-disk randomly selected coronal hole jets, and track the evolution of the jet-base. In each case we find that there is a minifilament present in the jet-base region prior to jet eruption. The minifilaments reside above a neutral line between majority-polarity and minority-polarity magnetic flux patches. HMI magnetograms show continuous flux cancelation at the neutral line between the opposite polarity flux patches. Persistent flux cancelation eventually destabilizes the field that holds the minifilament plasma. The erupting field reconnects with the neighboring far-reaching field and produces the jet spire. From our study, we conclude that flux cancelation is the fundamental process for triggering coronal hole jets. Other recent studies show that jets in quiet regions and active regions also are accompanied by flux cancelation at minifilament neutral lines (Panesar et al. 2016b, Sterling et al. 2017); therefore the same fundamental process - namely, magnetic flux cancelation - triggers at least many coronal jets in all regions of the Sun. Title: Solar Explosions Imager (SEIM): A Next-Generation High-Resolution and High-Cadence EUV Telescope for Unraveling Eruptive Solar Features Authors: Sterling, Alphonse C.; Moore, Ronald Lee; Winebarger, Amy R. Bibcode: 2018tess.conf11002S Altcode: We present a skeletal proposal for a space-based EUV telescope to fly on the Next Generation Solar Physics Mission (NGSPM). A primary motivation is to unravel physical processes leading to small-scale solar features, such as solar coronal jets, and the processes leading to larger eruptions as well. Recent evidence suggests that jets result from eruptions of small-scale filaments (size scale: ~1—a few arcsec), analogous to larger filament eruptions that drive CMEs, and it is plausible that the even-smaller-scale spicules (∼0′′.1) operate in a similar fashion. Therefore an instrument planned around the concept of observing jet features, but with the highest practical resolution and cadence, would be valuable for observing various erupting solar features on many size and time scales. Resolution and cadence should be comparable to or better than that of Hi-C, i.e. ≤0''.1 pixels and ≤10 s cadence. While no single instrument could span the entire needed data-set space needed to address fully these questions, the proposed instrument would complement first-rate instrumentation (namely, DKIST) expected to be in operation around the time of expected deployment. If resources permit, the proposed EUV instrument could be supplemented with additional instrumentation, or such additional instrumentation could be proposed as (a) separate effort(s). Especially complementary would be a photospheric magnetograph having ≤0''.1 pixels, ≤1-minute cadence, line-of-sight-field sensitivity of ≤10 G, and few-arc-minute FOV. (The SEIM concept has been presented as a WhitePaper with the same title to the NGSPM planning committee.) Title: Onset of the Magnetic Explosion in Solar Polar X-Ray Jets Authors: Moore, Ronald Lee; Sterling, Alphonse C.; Panesar, Navdeep Kaur Bibcode: 2018tess.conf30598M Altcode: We follow up on the Sterling et al (2015, Nature, 523, 437) discovery that nearly all solar polar X-ray jets are made by an explosive eruption of closed magnetic field carrying a miniature cool-plasma filament in its core. In the same X-ray and EUV movies used by Sterling et al (2015), we examine the onset and growth of the driving magnetic explosion in 15 of the 20 jets that they studied. We find evidence that: (1) in a large majority of polar X-ray jets, the runaway internal tether-cutting reconnection under the erupting minifilament flux rope starts after both the minifilament's rise and the spire-producing breakout reconnection have started; and (2) in a large minority, (a) before the eruption starts there is a current sheet between the explosive closed field and the ambient open field, and (b) the eruption starts with breakout reconnection at that current sheet. The observed sequence of events as the eruptions start and grow support the idea that the magnetic explosions that make polar X-ray jets work the same way as the much larger magnetic explosions that make a flare and coronal mass ejection (CME). That idea, and recent observations indicating that magnetic flux cancelation is the fundamental process that builds the field in and around the pre-jet minifilament and triggers that field's jet-driving explosion, together suggest that flux cancelation inside the magnetic arcade that explodes in a flare/CME eruption is usually the fundamental process that builds the explosive field in the core of the arcade and triggers that field's explosion. This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Science Program and the Heliophysics Guest Investigators Program. Title: MAG4's New Database of HMI Active-Region Vector Magnetograms: Sample Size and Initial Results for Major-Flare Forecasting Authors: Falconer, David Allen; Tiwari, Sanjiv K.; Moore, Ron L. Bibcode: 2018tess.conf41406F Altcode: We have developed a large-database method of forecasting an active region's (AR's) chance of producing a major flare (GOES M- or X-class) and its chance of producing a major CME (speed > 800 km/s) in the coming few days from a free-energy proxy - a proxy of the AR's free magnetic energy - measured from a magnetogram of the AR. We have named this forecasting tool MAG4 (for Magnetogram Forecast). In its present near-real-time operation mode, MAG4 forecasts each on-disk AR's rates of production of major flares and major CMEs in the coming few days, based on the observed major-flare and major-CME histories of 1,300 ARs observed within 30 degrees of disk center in MDI line-of-sight magnetograms. From the passages of these ARs across the 30-degree central disk, the presently-used MAG4 MDI database has the value of a free-energy proxy measured from 40,000 MDI magnetograms of these 1,300 ARs. We are now compiling a similar database of the about the same size for MAG4, but for HMI vector magnetograms that are of ARs observed within 45 degrees of disk center and that have been deprojected to disk center. This new MAG4 HMI database now has a wide variety of AR parameters measured from each of 40,000 deprojected HMI vector magnetograms of 900 ARs within 45 degrees of disk center (15 magnetograms of each AR per day during its passage across the 45-degree central disk). We present the MAG4 major-flare forecasting curves obtained from this new database for a few alternative free-energy proxies measured from either the vertical-field component or the horizontal-field component of the deprojected AR vector magnetograms. (The magnetogram's horizontal-field component more directly reflects the AR's free magnetic energy than does the magnetogram's vertical-field component.) By using our statistical method of measuring, via a skill score, whether the forecasting performance of one AR magnetogram parameter is significantly better than that of another, we show which free-energy proxy is the best major-flare predictor that we have found so far. Title: Birth of a Bipolar Active Region in a Small Solar Coronal Hole Authors: Adams, Mitzi; Panesar, Navdeep Kaur; Moore, Ronald L. Bibcode: 2018tess.conf20235A Altcode: We report on an the emergence of an anemone active region in a very small Title: Observations of Large Penumbral Jets from IRIS and Hinode Authors: Tiwari, Sanjiv K.; Moore, Ronald Lee; De Pontieu, Bart; Tarbell, Theodore D.; Panesar, Navdeep Kaur; Winebarger, Amy R.; Sterling, Alphonse C. Bibcode: 2018tess.conf40807T Altcode: Recent observations from Hinode (SOT/FG) revealed the presence of large penumbral jets (widths ≥ 500 km, larger than normal penumbral microjets, which have widths < 400 km) repeatedly occurring at the same locations in a sunspot penumbra, at the tail of a penumbral filament or where the tails of several penumbral filaments apparently converge (Tiwari et al. 2016, ApJ). These locations were observed to have mixed-polarity flux in Stokes-V images from SOT/FG. Large penumbral jets displayed direct signatures in AIA 1600, 304, 171, and 193 channels; thus they were heated to at least transition region temperatures. Because large jets could not be detected in AIA 94 Å, whether they had any coronal-temperature plasma remains unclear. In the present work, for another sunspot, we use IRIS Mg II k 2796 slit jaw images and spectra and magnetograms from Hinode SOT/FG and SOT/SP to examine: whether penumbral jets spin, similar to spicules and coronal jets in the quiet Sun and coronal holes; whether they stem from mixed-polarity flux; and whether they produce discernible coronal emission, especially in AIA 94 Å images. Title: Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets Authors: Moore, Ronald L.; Sterling, Alphonse C.; Panesar, Navdeep K. Bibcode: 2018ApJ...859....3M Altcode: 2018arXiv180512182M We follow up on the Sterling et al. discovery that nearly all polar coronal X-ray jets are made by an explosive eruption of a closed magnetic field carrying a miniature filament in its core. In the same X-ray and EUV movies used by Sterling et al., we examine the onset and growth of the driving magnetic explosion in 15 of the 20 jets that they studied. We find evidence that (1) in a large majority of polar X-ray jets, the runaway internal/tether-cutting reconnection under the erupting minifilament flux rope starts after both the minifilament’s rise and the spire-producing external/breakout reconnection have started; and (2) in a large minority, (a) before the eruption starts, there is a current sheet between the explosive closed field and the ambient open field, and (b) the eruption starts with breakout reconnection at that current sheet. The variety of event sequences in the eruptions supports the idea that the magnetic explosions that make polar X-ray jets work the same way as the much larger magnetic explosions that make a flare and coronal mass ejection (CME). That idea and recent observations indicating that magnetic flux cancellation is the fundamental process that builds the field in and around the pre-jet minifilament and triggers that field’s jet-driving explosion together suggest that flux cancellation inside the magnetic arcade that explodes in a flare/CME eruption is usually the fundamental process that builds the explosive field in the core of the arcade and triggers that field’s explosion. Title: Magnetic Flux Cancelation as the Trigger of Solar Coronal Jets in Coronal Holes Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2018ApJ...853..189P Altcode: 2018arXiv180105344P We investigate in detail the magnetic cause of minifilament eruptions that drive coronal-hole jets. We study 13 random on-disk coronal-hole jet eruptions, using high-resolution X-ray images from the Hinode/X-ray telescope(XRT), EUV images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), and magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). For all 13 events, we track the evolution of the jet-base region and find that a minifilament of cool (transition-region-temperature) plasma is present prior to each jet eruption. HMI magnetograms show that the minifilaments reside along a magnetic neutral line between majority-polarity and minority-polarity magnetic flux patches. These patches converge and cancel with each other, with an average cancelation rate of ∼0.6 × 1018 Mx hr-1 for all 13 jets. Persistent flux cancelation at the neutral line eventually destabilizes the minifilament field, which erupts outward and produces the jet spire. Thus, we find that all 13 coronal-hole-jet-driving minifilament eruptions are triggered by flux cancelation at the neutral line. These results are in agreement with our recent findings for quiet-region jets, where flux cancelation at the underlying neutral line triggers the minifilament eruption that drives each jet. Thus, from that study of quiet-Sun jets and this study of coronal-hole jets, we conclude that flux cancelation is the main candidate for triggering quiet-region and coronal-hole jets. Title: Theory and Transport of Nearly Incompressible Magnetohydrodynamic Turbulence. IV. Solar Coronal Turbulence Authors: Zank, G. P.; Adhikari, L.; Hunana, P.; Tiwari, S. K.; Moore, R.; Shiota, D.; Bruno, R.; Telloni, D. Bibcode: 2018ApJ...854...32Z Altcode: A new model describing the transport and evolution of turbulence in the quiet solar corona is presented. In the low plasma beta environment, transverse photospheric convective fluid motions drive predominantly quasi-2D (nonpropagating) turbulence in the mixed-polarity “magnetic carpet,” together with a minority slab (Alfvénic) component. We use a simplified sub-Alfvénic flow velocity profile to solve transport equations describing the evolution and dissipation of turbulence from 1\hspace{0.5em}{{t}}{{o}} 15 {R}⊙ (including the Alfvén surface). Typical coronal base parameters are used, although one model uses correlation lengths derived observationally by Abramenko et al., and the other assumes values 10 times larger. The model predicts that (1) the majority quasi-2D turbulence evolves from a balanced state at the coronal base to an imbalanced state, with outward fluctuations dominating, at and beyond the Alfvén surface, i.e., inward turbulent fluctuations are dissipated preferentially; (2) the initially imbalanced slab component remains imbalanced throughout the solar corona, being dominated by outwardly propagating Alfvén waves, and wave reflection is weak; (3) quasi-2D turbulence becomes increasingly magnetized, and beyond ∼ 6 {R}⊙ , the kinetic energy is mainly in slab fluctuations; (4) there is no accumulation of inward energy at the Alfvén surface; (5) inertial range quasi-2D rather than slab fluctuations are preferentially dissipated within ∼ 3 {R}⊙ ; and (6) turbulent dissipation of quasi-2D fluctuations is sufficient to heat the corona to temperatures ∼ 2× {10}6 K within 2 {R}⊙ , consistent with observations that suggest that the fast solar wind is accelerated most efficiently between ∼ 2\hspace{0.5em}{{a}}{{n}}{{d}} 4 {R}⊙ . Title: A Microfilament-Eruption Mechanism for Solar Spicules Authors: Sterling, A. C.; Moore, R. L. Bibcode: 2017AGUFMSH43A2791S Altcode: Recent studies indicate that solar coronal jets result from eruption of small-scale filaments, or "minifilaments" (Sterling et al. 2015, Nature, 523, 437; Panesar et al. ApJL, 832L, 7). In many aspects, these coronal jets appear to be small-scale versions of long-recognized large-scale solar eruptions that are often accompanied by eruption of a large-scale filament and that produce solar flares and coronal mass ejections (CMEs). In coronal jets, a jet-base bright point (JBP) that is often observed to accompany the jet and that sits on the magnetic neutral line from which the minifilament erupts, corresponds to the solar flare of larger-scale eruptions that occurs at the neutral line from which the large-scale filament erupts. Large-scale eruptions are relatively uncommon ( 1/day) and occur with relatively large-scale erupting filaments ( 10^5 km long). Coronal jets are more common (> 100s/day), but occur from erupting minifilaments of smaller size ( 10^4 km long). It is known that solar spicules are much more frequent (many millions/day) than coronal jets. Just as coronal jets are small-scale versions of large-scale eruptions, here we suggest that solar spicules might in turn be small-scale versions of coronal jets; we postulate that the spicules are produced by eruptions of ``microfilaments'' of length comparable to the width of observed spicules ( 300 km). A plot of the estimated number of the three respective phenomena (flares/CMEs, coronal jets, and spicules) occurring on the Sun at a given time, against the average sizes of erupting filaments, minifilaments, and the putative microfilaments, results in a size distribution that can be fit with a power-law within the estimated uncertainties. The counterparts of the flares of large-scale eruptions and the JBPs of jets might be weak, pervasive, transient brightenings observed in Hinode/CaII images, and the production of spicules by microfilament eruptions might explain why spicules spin, as do coronal jets. The expected small-scale neutral lines from which the microfilaments would be expected to erupt would be difficult to detect reliably with current instrumentation, but might be apparent with instrumentation of the near future. A summary of this work appears in Sterling and Moore 2016, ApJL, 829, L9. Title: Critical Magnetic Field Strengths for Unipolar Solar Coronal Plumes in Quiet Regions and Coronal Holes? Authors: Avallone, E. A.; Tiwari, S. K.; Panesar, N. K.; Moore, R. L. Bibcode: 2017AGUFMSH43A2797A Altcode: Coronal plumes are sporadic fountain-like structures that are bright in coronal emission. Each is a magnetic funnel rooted in a strong patch of dominant-polarity photospheric magnetic flux surrounded by a predominantly-unipolar magnetic network, either in a quiet region or a coronal hole. The heating processes that make plumes bright evidently involve the magnetic field in the base of the plume, but remain mysterious. Raouafi et al. (2014) inferred from observations that plume heating is a consequence of magnetic reconnection in the base, whereas Wang et al. (2016) showed that plume heating turns on/off from convection-driven convergence/divergence of the base flux. While both papers suggest that the base magnetic flux in their plumes is of mixed polarity, these papers provide no measurements of the abundance and strength of the evolving base flux or consider whether a critical magnetic field strength is required for a plume to become noticeably bright. To address plume production and evolution, we track the plume luminosity and the abundance and strength of the base magnetic flux over the lifetimes of six coronal plumes, using Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 171 Å images and SDO/Helioseismic and Magnetic Imager (HMI) line-of-sight magnetograms. Three of these plumes are in coronal holes, three are in quiet regions, and each plume exhibits a unipolar base flux. We track the base magnetic flux over each plume's lifetime to affirm that its convergence and divergence respectively coincide with the appearance and disappearance of the plume in 171 Å images. We tentatively find that plume formation requires enough convergence of the base flux to surpass a field strength of ∼300-500 Gauss, and that quiet Sun and coronal-hole plumes both exhibit the same behavior in the response of their luminosity in 171 Å to the strength of the magnetic field in the base. Title: Dynamic Solar Coronal Jets occurring in a Near-Limb Active Region Authors: Velasquez, J.; Sterling, A. C.; Falconer, D. A.; Moore, R. L.; Panesar, N. K. Bibcode: 2017AGUFMSH43A2792V Altcode: Coronal Jets are long, narrow columns of plasma ejected from the lower solar atmosphere into the corona and observed at coronal wavelengths. In this study, we observe a series of coronal jets occurring in NOAA active region (AR) 12473 on 2015 December 30. At that time the AR was approaching the Sun's west limb, allowing for observation of the jets in profile, contrasting with our recent studies of on-disk active region jets (Sterling et al. 2016, ApJ, 821, 100; and 2017, ApJ, 844, 28). We observe the jets using X-ray images from Hinode's X-Ray Telescope (XRT) and EUV images from the Solar Dynamic Observatory's (SDO) Atmospheric Imaging Assembly (AIA). Here, we investigate the dynamic trajectories of about 9 jets, by measuring the distance between the jet base and the leading edge of the erupting jet (i.e., the jet length) as a function of time, when observed in 304 Angstrom AIA images. All of the selected jets are concurrently visible in X-rays, and thus we are measuring properties of the chromospheric-transition region "cool component" of X-ray jets; in most cases, the appearance of the jets, such as the length of their spire, differs substantially between the X-ray and EUV 304 Angstrom images. For our selection of jets, we find that in the 304 Angstrom images many of them spin as they extend. Most of those in our selection do not make coronal mass ejections (CMEs); on average our jets have outward velocities of about 126 km/s, average maximum lengths of 84,000 km, and average lifetimes of 38 min. These values fall in the range of outward velocities and lifetimes found by Panesar et al. (2016, ApJ, 822, L23) for active-region 304 Angstrom jets that did not make CMEs. These values are also comparable to those found by Moschou et al. (2013, Solar Phys, 284, 427) for a selection of quiet Sun and coronal hole 304 Angstrom jets. One of our selected jets did make a CME, and it has outward velocity of about 240 km/s, consistent with the Panesar et al. (2016) results for CME-producing jets. Title: Magnetic Flux Cancellation as the Trigger of Solar Coronal Jets Authors: McGlasson, R.; Panesar, N. K.; Sterling, A. C.; Moore, R. L. Bibcode: 2017AGUFMSH43A2796M Altcode: Coronal jets are narrow eruptions in the solar corona, and are often observed in extreme ultraviolet (EUV) and X-ray images. They occur everywhere on the solar disk: in active regions, quiet regions, and coronal holes (Raouafi et al. 2016). Recent studies indicate that most coronal jets in quiet regions and coronal holes are driven by the eruption of a minifilament (Sterling et al. 2015), and that this eruption follows flux cancellation at the magnetic neutral line under the pre-eruption minifilament (Panesar et al. 2016). We confirm this picture for a large sample of jets in quiet regions and coronal holes using multithermal (304 Å 171 Å, 193 Å, and 211 Å) extreme ultraviolet (EUV) images from the Solar Dynamics Observatory (SDO) /Atmospheric Imaging Assembly (AIA) and line-of-sight magnetograms from the SDO /Helioseismic and Magnetic Imager (HMI). We report observations of 60 randomly selected jet eruptions. We have analyzed the magnetic cause of these eruptions and measured the base size and the duration of each jet using routines in SolarSoft IDL. By examining the evolutionary changes in the magnetic field before, during, and after jet eruption, we found that each of these jets resulted from minifilament eruption triggered by flux cancellation at the neutral line. In agreement with the above studies, we found our jets to have an average base diameter of 7600 ± 2700 km and an average duration of 9.0 ± 3.6 minutes. These observations confirm that minifilament eruption is the driver and magnetic flux cancellation is the primary trigger mechanism for nearly all coronal hole and quiet region coronal jet eruptions. Title: Invisibility of Solar Active Region Umbra-to-Umbra Coronal Loops: New Evidence that Magnetoconvection Drives Solar-Stellar Coronal Heating Authors: Tiwari, S. K.; Thalmann, J. K.; Panesar, N. K.; Moore, R. L.; Winebarger, A. R. Bibcode: 2017AGUFMSH43A2789T Altcode: Coronal heating generally increases with increasing magnetic field strength: the EUV/X-ray corona in active regions is 10-100 times more luminous and 2-4 times hotter than that in quiet regions and coronal holes, which are heated to only about 1.5 MK, and have fields that are 10-100 times weaker than that in active regions. From a comparison of a nonlinear force-free model of the three-dimensional active region coronal field to observed extreme-ultraviolet loops, we find that (1) umbra-to-umbra coronal loops, despite being rooted in the strongest magnetic flux, are invisible, and (2) the brightest loops have one foot in an umbra or penumbra and the other foot in another sunspot's penumbra or in unipolar or mixed-polarity plage. The invisibility of umbra-to-umbra loops is new evidence that magnetoconvection drives solar-stellar coronal heating: evidently, the strong umbral field at both ends quenches the magnetoconvection and hence the heating. Our results from EUV observations and nonlinear force-free modeling of coronal magnetic field imply that, for any coronal loop on the Sun or on any other convective star, as long as the field can be braided by convection in at least one loop foot, the stronger the field in the loop, the stronger the coronal heating. Title: Origin of Pre-Coronal-Jet Minifilaments: Flux Cancellation Authors: Panesar, N. K.; Sterling, A. C.; Moore, R. L. Bibcode: 2017AGUFMSH41C..03P Altcode: We recently investigated the triggering mechanism of ten quiet-region coronal jet eruptions and found that magnetic flux cancellation at the neutral line of minifilaments is the main cause of quiet-region jet eruptions (Panesar et al 2016). However, what leads to the formation of the pre-jet minifilaments remained unknown. In the present work, we study the longer-term evolution of the magnetic field that leads to the formation of pre-jet minifilaments by using SDO/AIA intensity images and concurrent line of sight SDO/HMI magnetograms. We find that each of the ten pre-jet minifilaments formed due to progressive flux cancellation between the minority-polarity and majority-polarity flux patches (with a minority-polarity flux loss of 10% - 40% prior to minifilament birth). Apparently, the flux cancellation between the opposite polarity flux patches builds a highly-sheared field at the magnetic neutral line, and that field holds the cool transition region minifilament plasma. Even after the formation of minifilaments, the flux continues to cancel, making the minifilament body more thick and prominent. Further flux cancellation between the opposite-flux patches leads to the minifilament eruption and a resulting jet. From these observations, we infer that flux cancellation is usually the process that builds up the sheared and twisted field in pre-jet minifilaments, and that triggers it to erupt and drive a jet. Title: Coronal Heating and the Magnetic Field in Solar Active Regions Authors: Falconer, D. A.; Tiwari, S. K.; Winebarger, A. R.; Moore, R. L. Bibcode: 2017AGUFMSH43A2790F Altcode: A strong dependence of active-region (AR) coronal heating on the magnetic field is demonstrated by the strong correlation of AR X-ray luminosity with AR total magnetic flux (Fisher et al 1998 ApJ). AR X-ray luminosity is also correlated with AR length of strong-shear neutral line in the photospheric magnetic field (Falconer 1997). These two whole-AR magnetic parameters are also correlated with each other. From 150 ARs observed within 30 heliocentric degrees from disk center by AIA and HMI on SDO, using AR luminosity measured from the hot component of the AIA 94 Å band (Warren et al 2012, ApJ) near the time of each of 3600 measured HMI vector magnetograms of these ARs and a wide selection of whole-AR magnetic parameters from each vector magnetogram after it was deprojected to disk center, we find: (1) The single magnetic parameter having the strongest correlation with AR 94-hot luminosity is the length of strong-field neutral line. (2) The two-parameter combination having the strongest still-stronger correlation with AR 94-hot luminosity is a combination of AR total magnetic flux and AR neutral-line length weighted by the vertical-field gradient across the neutral line. We interpret these results to be consistent with the results of both Fisher et al (1998) and Falconer (1997), and with the correlation of AR coronal loop heating with loop field strength recently found by Tiwari et al (2017, ApJ Letters). Our interpretation is that, in addition to depending strongly on coronal loop field strength, AR coronal heating has a strong secondary positive dependence on the rate of flux cancelation at neutral lines at coronal loop feet. This work was funded by the Living With a Star Science and Heliophysics Guest Investigators programs of NASA's Heliophysics Division. Title: Onset of a Large Ejective Solar Eruption from a Typical Coronal-jet-base Field Configuration Authors: Joshi, Navin Chandra; Sterling, Alphonse C.; Moore, Ronald L.; Magara, Tetsuya; Moon, Yong-Jae Bibcode: 2017ApJ...845...26J Altcode: 2017arXiv170609176J Utilizing multiwavelength observations and magnetic field data from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), SDO/Helioseismic and Magnetic Imager (HMI), the Geostationary Operational Environmental Satellite (GOES), and RHESSI, we investigate a large-scale ejective solar eruption of 2014 December 18 from active region NOAA 12241. This event produced a distinctive “three-ribbon” flare, having two parallel ribbons corresponding to the ribbons of a standard two-ribbon flare, and a larger-scale third quasi-circular ribbon offset from the other two. There are two components to this eruptive event. First, a flux rope forms above a strong-field polarity inversion line and erupts and grows as the parallel ribbons turn on, grow, and spread apart from that polarity inversion line; this evolution is consistent with the mechanism of tether-cutting reconnection for eruptions. Second, the eruption of the arcade that has the erupting flux rope in its core undergoes magnetic reconnection at the null point of a fan dome that envelops the erupting arcade, resulting in formation of the quasi-circular ribbon; this is consistent with the breakout reconnection mechanism for eruptions. We find that the parallel ribbons begin well before (∼12 minutes) the onset of the circular ribbon, indicating that tether-cutting reconnection (or a non-ideal MHD instability) initiated this event, rather than breakout reconnection. The overall setup for this large-scale eruption (diameter of the circular ribbon ∼105 km) is analogous to that of coronal jets (base size ∼104 km), many of which, according to recent findings, result from eruptions of small-scale “minifilaments.” Thus these findings confirm that eruptions of sheared-core magnetic arcades seated in fan-spine null-point magnetic topology happen on a wide range of size scales on the Sun. Title: A new method to quantify and reduce projection error in whole-solar-active-region parameters measured from vector magnetograms Authors: Falconer, David; Tiwari, Sanjiv K.; Moore, Ronald L.; Khazanov, Igor Bibcode: 2017SPD....4811107F Altcode: Projection error limits the use of vector magnetograms of active regions (ARs) far from disk center. For ARs observed up to 60o from disk center, we demonstrate a method of measuring and reducing the projection error in the magnitude of any whole-AR parameter derived from a vector magnetogram that has been deprojected to disk center. The method assumes that the center-to-limb curve of the average of the parameter’s absolute values measured from the disk passage of a large number of ARs and normalized to each AR’s absolute value of the parameter at central meridian, gives the average fractional projection error at each radial distance from disk center. To demonstrate the method, we use a large set of large-flux ARs and apply the method to a whole-AR parameter that is among the simplest to measure: whole-AR magnetic flux. We measure 30,845 SDO/HMI vector magnetograms covering the disk passage of 272 large-flux ARs, each having whole-AR flux >1022 Mx. We obtain the center-to-limb radial-distance run of the average projection error in measured whole-AR flux from a Chebyshev fit to the radial-distance plot of the 30,845 normalized measured values. The average projection error in the measured whole-AR flux of an AR at a given radial distance is removed by multiplying the measured flux by the correction factor given by the fit. The correction is important for both the study of evolution of ARs and for improving the accuracy of forecasting an AR’s major flare/CME productivity. We will also show corrections for other whole-AR parameters, especially AR free-energy proxies. Title: Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets Authors: Moore, Ronald L.; Sterling, Alphonse C.; Panesar, Navdeep Bibcode: 2017SPD....4820006M Altcode: We examine the onset of the driving magnetic explosion in 15 random polar coronal X-ray jets. Each eruption is observed in a coronal X-ray movie from Hinode and in a coronal EUV movie from Solar Dynamics Observatory. Contrary to the Sterling et al (2015, Nature, 523, 437) scenario for minifilament eruptions that drive polar coronal jets, these observations indicate: (1) in most polar coronal jets (a) the runaway internal tether-cutting reconnection under the erupting minifilament flux rope starts after the spire-producing breakout reconnection starts, not before it, and (b) aleady at eruption onset, there is a current sheet between the explosive closed magnetic field and ambient open field; and (2) the minifilament-eruption magnetic explosion often starts with the breakout reconnection of the outside of the magnetic arcade that carries the minifilament in its core. On the other hand, the diversity of the observed sequences of occurrence of events in the jet eruptions gives further credence to the Sterlling et al (2015, Nature, 523, 437) idea that the magnetic explosions that make a polar X-ray jet work the same way as the much larger magnetic explosions that make and flare and CME. We point out that this idea, and recent observations indicating that magnetic flux cancelation is the fundamental process that builds the field in and around pre-jet minifilaments and triggers the jet-driving magnetic explosion, together imply that usually flux cancelation inside the arcade that explodes in a flare/CME eruption is the fundamental process that builds the explosive field and triggers the explosion.This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through its Living With a Star Targeted Research and Technology Program, its Heliophsyics Guest Investigators Program, and the Hinode Project. Title: Active Region Jets II: Triggering and Evolution of Violent Jets Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David; Panesar, Navdeep K.; Martinez, Francisco Bibcode: 2017SPD....4830403S Altcode: We study a series of X-ray-bright, rapidly evolving active-region coronal jets outside the leading sunspot of AR 12259, using Hinode/XRT, SDO/AIA and HMI, and IRIS/SJ data. The detailed evolution of such rapidly evolving “violent” jets remained a mystery after our previous investigation of active region jets (Sterling et al. 2016, ApJ, 821, 100). The jets we investigate here erupt from three localized subregions, each containing a rapidly evolving (positive) minority-polarity magnetic-flux patch bathed in a (majority) negative-polarity magnetic-flux background. At least several of the jets begin with eruptions of what appear to be thin (thickness ∼<2‧‧) miniature-filament (minifilament) “strands” from a magnetic neutral line where magnetic flux cancelation is ongoing, consistent with the magnetic configuration presented for coronal-hole jets in Sterling et al. (2015, Nature, 523, 437). For some jets strands are difficult/ impossible to detect, perhaps due to their thinness, obscuration by surrounding bright or dark features, or the absence of erupting cool-material minifilaments in those jets. Tracing in detail the flux evolution in one of the subregions, we find bursts of strong jetting occurring only during times of strong flux cancelation. Averaged over seven jetting episodes, the cancelation rate was ~1.5×10^19 Mx/hr. An average flux of ~5×10^18 Mx canceled prior to each episode, arguably building up ~10^28—10^29 ergs of free magnetic energy per jet. From these and previous observations, we infer that flux cancelation is the fundamental process responsible for the pre-eruption buildup and triggering of at least many jets in active regions, quiet regions, and coronal holes. Title: Flux Cancelation as the trigger of quiet-region coronal jet eruptions Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2017SPD....4830402P Altcode: Coronal jets are frequent transient features on the Sun, observed in EUV and X-ray emissions. They occur in active regions, quiet Sun and coronal holes, and appear as a bright spire with base brightenings. Recent studies show that many coronal jets are driven by the eruption of a minifilament. Here we investigate the magnetic cause of jet-driving minifilament eruptions. We study ten randomly-found on-disk quiet-region coronal jets using SDO/AIA intensity images and SDO/HMI magnetograms. For all ten events, we track the evolution of the jet-base region and find that (a) a cool (transition-region temperature) minifilament is present prior to each jet eruption; (b) the pre-eruption minifilament resides above the polarity-inversion line between majority-polarity and minority-polarity magnetic flux patches; (c) the opposite-polarity flux patches converge and cancel with each other; (d) the ongoing cancelation between the majority-polarity and minority-polarity flux patches eventually destabilizes the field holding the minifilament to erupt outwards; (e) the envelope of the erupting field barges into ambient oppositely-directed far-reaching field and undergoes external reconnection (interchange reconnection); (f) the external reconnection opens the envelope field and the minifilament field inside, allowing reconnection-heated hot material and cool minifilament material to escape along the reconnected far-reaching field, producing the jet spire. In summary, we found that each of our ten jets resulted from a minifilament eruption during flux cancelation at the magnetic neutral line under the pre-eruption minifilament. These observations show that flux cancelation is usually the trigger of quiet-region coronal jet eruptions. Title: Magnetic Flux Cancellation as the Origin of Solar Quiet-region Pre-jet Minifilaments Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2017ApJ...844..131P Altcode: 2017arXiv170609079P We investigate the origin of 10 solar quiet-region pre-jet minifilaments, using EUV images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and magnetograms from the SDO Helioseismic and Magnetic Imager (HMI). We recently found that quiet-region coronal jets are driven by minifilament eruptions, where those eruptions result from flux cancellation at the magnetic neutral line under the minifilament. Here, we study the longer-term origin of the pre-jet minifilaments themselves. We find that they result from flux cancellation between minority-polarity and majority-polarity flux patches. In each of 10 pre-jet regions, we find that opposite-polarity patches of magnetic flux converge and cancel, with a flux reduction of 10%-40% from before to after the minifilament appears. For our 10 events, the minifilaments exist for periods ranging from 1.5 hr to 2 days before erupting to make a jet. Apparently, the flux cancellation builds a highly sheared field that runs above and traces the neutral line, and the cool transition region plasma minifilament forms in this field and is suspended in it. We infer that the convergence of the opposite-polarity patches results in reconnection in the low corona that builds a magnetic arcade enveloping the minifilament in its core, and that the continuing flux cancellation at the neutral line finally destabilizes the minifilament field so that it erupts and drives the production of a coronal jet. Thus, our observations strongly support that quiet-region magnetic flux cancellation results in both the formation of the pre-jet minifilament and its jet-driving eruption. Title: Evidence from IRIS that Sunspot Large Penumbral Jets Spin Authors: Tiwari, Sanjiv K.; Moore, Ronald L.; De Pontieu, Bart; Tarbell, Theodore D.; Panesar, Navdeep K.; Winebarger, Amy; Sterling, Alphonse C. Bibcode: 2017SPD....4810506T Altcode: Recent observations from {\it Hinode} (SOT/FG) revealed the presence of large penumbral jets (widths $\ge$500 km, larger than normal penumbral microjets, which have widths $<$ 400 km) repeatedly occurring at the same locations in a sunspot penumbra, at the tail of a filament or where the tails of several penumbral filaments apparently converge (Tiwari et al. 2016, ApJ). These locations were observed to have mixed-polarity flux in Stokes-V images from SOT/FG. Large penumbral jets displayed direct signatures in AIA 1600, 304, 171, and 193 channels; thus they were heated to at least transition region temperatures. Because large jets could not be detected in AIA 94 \AA, whether they had any coronal-temperature plasma remains unclear. In the present work, for another sunspot, we use IRIS Mg II k 2796 Å slit jaw images and spectra and magnetograms from Hinode SOT/FG and SOT/SP to examine: whether penumbral jets spin, similar to spicules and coronal jets in the quiet Sun and coronal holes; whether they stem from mixed-polarity flux; and whether they produce discernible coronal emission, especially in AIA 94 Å images. The few large penumbral jets for which we have IRIS spectra show evidence of spin. If these have mixed-polarity at their base, then they might be driven the same way as coronal jets and CMEs. Title: Babcock Redux: An Amendment of Babcock's Schematic of the Sun's Magnetic Cycle Authors: Moore, Ronald L.; Cirtain, Jonathan W.; Sterling, Alphonse C. Bibcode: 2017SPD....4811103M Altcode: We amend Babcock's original scenario for the global dynamo process that sustains the Sun's 22-year magnetic cycle. The amended scenario fits post-Babcock observed features of the magnetic activity cycle and convection zone, and is based on ideas of Spruit & Roberts (1983, Nature, 304, 401) about magnetic flux tubes in the convection zone. A sequence of four schematic cartoons lays out the proposed evolution of the global configuration of the magnetic field above, in, and at the bottom of the convection zone through sunspot Cycle 23 and into Cycle 24. Three key elements of the amended scenario are: (1) as the net following-polarity magnetic field from the sunspot-region Ω-loop fields of an ongoing sunspot cycle is swept poleward to cancel and replace the opposite-polarity polar-cap field from the previous sunspot cycle, it remains connected to the ongoing sunspot cycle's toroidal source-field band at the bottom of the convection zone; (2) topological pumping by the convection zone's free convection keeps the horizontal extent of the poleward-migrating following-polarity field pushed to the bottom, forcing it to gradually cancel and replace old horizontal field below it that connects the ongoing-cycle source-field band to the previous-cycle polar-cap field; (3) in each polar hemisphere, by continually shearing the poloidal component of the settling new horizontal field, the latitudinal differential rotation low in the convection zone generates the next-cycle source-field band poleward of the ongoing-cycle band. The amended scenario is a more-plausible version of Babcock's scenario, and its viability can be explored by appropriate kinematic flux-transport solar-dynamo simulations. A paper giving a full description of our dynamo scenario is posted on arXiv (http://arxiv.org/abs/1606.05371).This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program and the Hinode Project. Title: Solar Active Region Coronal Jets. II. Triggering and Evolution of Violent Jets Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Panesar, Navdeep K.; Martinez, Francisco Bibcode: 2017ApJ...844...28S Altcode: 2017arXiv170503040S We study a series of X-ray-bright, rapidly evolving active region coronal jets outside the leading sunspot of AR 12259, using Hinode/X-ray telescope, Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI), and Interface Region Imaging Spectrograph (IRIS) data. The detailed evolution of such rapidly evolving “violent” jets remained a mystery after our previous investigation of active region jets. The jets we investigate here erupt from three localized subregions, each containing a rapidly evolving (positive) minority-polarity magnetic-flux patch bathed in a (majority) negative-polarity magnetic-flux background. At least several of the jets begin with eruptions of what appear to be thin (thickness ≲ 2\prime\prime ) miniature-filament (minifilament) “strands” from a magnetic neutral line where magnetic flux cancelation is ongoing, consistent with the magnetic configuration presented for coronal-hole jets in Sterling et al. (2016). Some jets strands are difficult/impossible to detect, perhaps due to, e.g., their thinness, obscuration by surrounding bright or dark features, or the absence of erupting cool-material minifilaments in those jets. Tracing in detail the flux evolution in one of the subregions, we find bursts of strong jetting occurring only during times of strong flux cancelation. Averaged over seven jetting episodes, the cancelation rate was ∼ 1.5× {10}19 Mx hr-1. An average flux of ∼ 5× {10}18 Mx canceled prior to each episode, arguably building up ∼1028-1029 erg of free magnetic energy per jet. From these and previous observations, we infer that flux cancelation is the fundamental process responsible for the pre-eruption build up and triggering of at least many jets in active regions, quiet regions, and coronal holes. Title: New Evidence that Magnetoconvection Drives Solar-Stellar Coronal Heating Authors: Tiwari, Sanjiv K.; Thalmann, Julia K.; Panesar, Navdeep K.; Moore, Ronald L.; Winebarger, Amy R. Bibcode: 2017ApJ...843L..20T Altcode: 2017arXiv170608035T How magnetic energy is injected and released in the solar corona, keeping it heated to several million degrees, remains elusive. Coronal heating generally increases with increasing magnetic field strength. From a comparison of a nonlinear force-free model of the three-dimensional active region coronal field to observed extreme-ultraviolet loops, we find that (1) umbra-to-umbra coronal loops, despite being rooted in the strongest magnetic flux, are invisible, and (2) the brightest loops have one foot in an umbra or penumbra and the other foot in another sunspot’s penumbra or in unipolar or mixed-polarity plage. The invisibility of umbra-to-umbra loops is new evidence that magnetoconvection drives solar-stellar coronal heating: evidently, the strong umbral field at both ends quenches the magnetoconvection and hence the heating. Broadly, our results indicate that depending on the field strength in both feet, the photospheric feet of a coronal loop on any convective star can either engender or quench coronal heating in the loop’s body. Title: The Triggering Mechanism of Coronal Jets and CMEs: Flux Cancelation Authors: Panesar, Navdeep K.; Sterling, Alphonse; Moore, Ronald Bibcode: 2017shin.confE..27P Altcode: Recent investigations (e.g. Sterling et al 2015, Panesar et al 2016) show that coronal jets are driven by the eruption of a small-scale filament (10,000 - 20,000 km long, called a minifilament) following magnetic flux cancelation at the neutral line underneath the minifilament. Minifilament eruptions appear to be analogous to larger-scale solar filament eruptions: they both reside, before the eruption, in the highly sheared field between the adjacent opposite-polarity magnetic flux patches (neutral line); jet-producing minifilament and larger-scale solar filament first show a slow-rise, followed by a fast-rise as they erupt; during the jet-producing minifilament eruption a jet bright point (JBP) appears at the location where the minifilament was rooted before the eruption, analogous to the situation with CME-producing larger-scale filament eruptions where a solar flare arcade forms during the filament eruption along the neutral line along which the filament resided prior to its eruption. In the present study we investigate the triggering mechanism of CME-producing large solar filament eruptions, and find that enduring flux cancelation at the neutral line of the filaments often triggers their eruptions. This corresponds to the finding that persistent flux cancelation at the neutral is the cause of jet-producing minifilament eruptions. Thus our observations support coronal jets being miniature version of CMEs. Title: Probing the W tb vertex structure in t-channel single-top-quark production and decay in pp collisions at √{s}=8 TeV with the ATLAS detector Authors: Aaboud, M.; Aad, G.; Abbott, B.; Abdallah, J.; Abdinov, O.; Abeloos, B.; AbouZeid, O. S.; Abraham, N. L.; Abramowicz, H.; Abreu, H.; Abreu, R.; Abulaiti, Y.; Acharya, B. S.; Adachi, S.; Adamczyk, L.; Adams, D. L.; Adelman, J.; Adomeit, S.; Adye, T.; Affolder, A. A.; Agatonovic-Jovin, T.; Aguilar-Saavedra, J. A.; Ahlen, S. P.; Ahmadov, F.; Aielli, G.; Akerstedt, H.; Åkesson, T. P. A.; Akimov, A. V.; Alberghi, G. L.; Albert, J.; Albrand, S.; Verzini, M. J. Alconada; Aleksa, M.; Aleksandrov, I. N.; Alexa, C.; Alexander, G.; Alexopoulos, T.; Alhroob, M.; Ali, B.; Aliev, M.; Alimonti, G.; Alison, J.; Alkire, S. P.; Allbrooke, B. M. M.; Allen, B. W.; Allport, P. P.; Aloisio, A.; Alonso, A.; Alonso, F.; Alpigiani, C.; Alshehri, A. A.; Alstaty, M.; Gonzalez, B. Alvarez; Piqueras, D. Álvarez; Alviggi, M. G.; Amadio, B. T.; Coutinho, Y. Amaral; Amelung, C.; Amidei, D.; Santos, S. P. Amor Dos; Amorim, A.; Amoroso, S.; Amundsen, G.; Anastopoulos, C.; Ancu, L. S.; Andari, N.; Andeen, T.; Anders, C. F.; Anders, J. K.; Anderson, K. J.; Andreazza, A.; Andrei, V.; Angelidakis, S.; Angelozzi, I.; Angerami, A.; Anghinolfi, F.; Anisenkov, A. V.; Anjos, N.; Annovi, A.; Antel, C.; Antonelli, M.; Antonov, A.; Antrim, D. J.; Anulli, F.; Aoki, M.; Bella, L. Aperio; Arabidze, G.; Arai, Y.; Araque, J. P.; Ferraz, V. Araujo; Arce, A. T. H.; Arduh, F. A.; Arguin, J. -F.; Argyropoulos, S.; Arik, M.; Armbruster, A. J.; Armitage, L. J.; Arnaez, O.; Arnold, H.; Arratia, M.; Arslan, O.; Artamonov, A.; Artoni, G.; Artz, S.; Asai, S.; Asbah, N.; Ashkenazi, A.; Åsman, B.; Asquith, L.; Assamagan, K.; Astalos, R.; Atkinson, M.; Atlay, N. B.; Augsten, K.; Avolio, G.; Axen, B.; Ayoub, M. K.; Azuelos, G.; Baak, M. A.; Baas, A. E.; Baca, M. J.; Bachacou, H.; Bachas, K.; Backes, M.; Backhaus, M.; Bagiacchi, P.; Bagnaia, P.; Bai, Y.; Baines, J. T.; Bajic, M.; Baker, O. K.; Baldin, E. M.; Balek, P.; Balestri, T.; Balli, F.; Balunas, W. K.; Banas, E.; Banerjee, Sw.; Bannoura, A. A. E.; Barak, L.; Barberio, E. L.; Barberis, D.; Barbero, M.; Barillari, T.; Barisits, M. -S.; Barklow, T.; Barlow, N.; Barnes, S. L.; Barnett, B. M.; Barnett, R. M.; Barnovska-Blenessy, Z.; Baroncelli, A.; Barone, G.; Barr, A. J.; Navarro, L. Barranco; Barreiro, F.; da Costa, J. Barreiro Guimarães; Bartoldus, R.; Barton, A. E.; Bartos, P.; Basalaev, A.; Bassalat, A.; Bates, R. L.; Batista, S. J.; Batley, J. R.; Battaglia, M.; Bauce, M.; Bauer, F.; Bawa, H. S.; Beacham, J. B.; Beattie, M. D.; Beau, T.; Beauchemin, P. H.; Bechtle, P.; Beck, H. P.; Becker, K.; Becker, M.; Beckingham, M.; Becot, C.; Beddall, A. J.; Beddall, A.; Bednyakov, V. A.; Bedognetti, M.; Bee, C. P.; Beemster, L. J.; Beermann, T. A.; Begel, M.; Behr, J. K.; Bell, A. S.; Bella, G.; Bellagamba, L.; Bellerive, A.; Bellomo, M.; Belotskiy, K.; Beltramello, O.; Belyaev, N. L.; Benary, O.; Benchekroun, D.; Bender, M.; Bendtz, K.; Benekos, N.; Benhammou, Y.; Noccioli, E. Benhar; Benitez, J.; Benjamin, D. P.; Bensinger, J. R.; Bentvelsen, S.; Beresford, L.; Beretta, M.; Berge, D.; Kuutmann, E. Bergeaas; Berger, N.; Beringer, J.; Berlendis, S.; Bernard, N. R.; Bernius, C.; Bernlochner, F. U.; Berry, T.; Berta, P.; Bertella, C.; Bertoli, G.; Bertolucci, F.; Bertram, I. A.; Bertsche, C.; Bertsche, D.; Besjes, G. J.; Bylund, O. Bessidskaia; Bessner, M.; Besson, N.; Betancourt, C.; Bethani, A.; Bethke, S.; Bevan, A. J.; Bianchi, R. M.; Bianco, M.; Biebel, O.; Biedermann, D.; Bielski, R.; Biesuz, N. V.; Biglietti, M.; De Mendizabal, J. Bilbao; Billoud, T. R. V.; Bilokon, H.; Bindi, M.; Bingul, A.; Bini, C.; Biondi, S.; Bisanz, T.; Bjergaard, D. M.; Black, C. W.; Black, J. E.; Black, K. M.; Blackburn, D.; Blair, R. E.; Blazek, T.; Bloch, I.; Blocker, C.; Blue, A.; Blum, W.; Blumenschein, U.; Blunier, S.; Bobbink, G. J.; Bobrovnikov, V. S.; Bocchetta, S. S.; Bocci, A.; Bock, C.; Boehler, M.; Boerner, D.; Bogaerts, J. A.; Bogavac, D.; Bogdanchikov, A. G.; Bohm, C.; Boisvert, V.; Bokan, P.; Bold, T.; Boldyrev, A. S.; Bomben, M.; Bona, M.; Boonekamp, M.; Borisov, A.; Borissov, G.; Bortfeldt, J.; Bortoletto, D.; Bortolotto, V.; Bos, K.; Boscherini, D.; Bosman, M.; Sola, J. D. Bossio; Boudreau, J.; Bouffard, J.; Bouhova-Thacker, E. V.; Boumediene, D.; Bourdarios, C.; Boutle, S. K.; Boveia, A.; Boyd, J.; Boyko, I. R.; Bracinik, J.; Brandt, A.; Brandt, G.; Brandt, O.; Bratzler, U.; Brau, B.; Brau, J. E.; Madden, W. D. Breaden; Brendlinger, K.; Brennan, A. J.; Brenner, L.; Brenner, R.; Bressler, S.; Bristow, T. M.; Britton, D.; Britzger, D.; Brochu, F. M.; Brock, I.; Brock, R.; Brooijmans, G.; Brooks, T.; Brooks, W. K.; Brosamer, J.; Brost, E.; Broughton, J. H.; de Renstrom, P. A. Bruckman; Bruncko, D.; Bruneliere, R.; Bruni, A.; Bruni, G.; Bruni, L. S.; Brunt, BH; Bruschi, M.; Bruscino, N.; Bryant, P.; Bryngemark, L.; Buanes, T.; Buat, Q.; Buchholz, P.; Buckley, A. G.; Budagov, I. A.; Buehrer, F.; Bugge, M. K.; Bulekov, O.; Bullock, D.; Burckhart, H.; Burdin, S.; Burgard, C. D.; Burger, A. M.; Burghgrave, B.; Burka, K.; Burke, S.; Burmeister, I.; Burr, J. T. P.; Busato, E.; Büscher, D.; Büscher, V.; Bussey, P.; Butler, J. M.; Buttar, C. M.; Butterworth, J. M.; Butti, P.; Buttinger, W.; Buzatu, A.; Buzykaev, A. R.; Urbán, S. Cabrera; Caforio, D.; Cairo, V. M.; Cakir, O.; Calace, N.; Calafiura, P.; Calandri, A.; Calderini, G.; Calfayan, P.; Callea, G.; Caloba, L. P.; Lopez, S. Calvente; Calvet, D.; Calvet, S.; Calvet, T. P.; Toro, R. Camacho; Camarda, S.; Camarri, P.; Cameron, D.; Armadans, R. Caminal; Camincher, C.; Campana, S.; Campanelli, M.; Camplani, A.; Campoverde, A.; Canale, V.; Canepa, A.; Bret, M. Cano; Cantero, J.; Cao, T.; Garrido, M. D. M. Capeans; Caprini, I.; Caprini, M.; Capua, M.; Carbone, R. M.; Cardarelli, R.; Cardillo, F.; Carli, I.; Carli, T.; Carlino, G.; Carlson, B. T.; Carminati, L.; Carney, R. M. D.; Caron, S.; Carquin, E.; Carrillo-Montoya, G. D.; Carter, J. R.; Carvalho, J.; Casadei, D.; Casado, M. P.; Casolino, M.; Casper, D. W.; Castaneda-Miranda, E.; Castelijn, R.; Castelli, A.; Gimenez, V. Castillo; Castro, N. F.; Catinaccio, A.; Catmore, J. R.; Cattai, A.; Caudron, J.; Cavaliere, V.; Cavallaro, E.; Cavalli, D.; Cavalli-Sforza, M.; Cavasinni, V.; Ceradini, F.; Alberich, L. Cerda; Cerqueira, A. S.; Cerri, A.; Cerrito, L.; Cerutti, F.; Cervelli, A.; Cetin, S. A.; Chafaq, A.; Chakraborty, D.; Chan, S. K.; Chan, Y. L.; Chang, P.; Chapman, J. D.; Charlton, D. G.; Chatterjee, A.; Chau, C. C.; Barajas, C. A. Chavez; Che, S.; Cheatham, S.; Chegwidden, A.; Chekanov, S.; Chekulaev, S. V.; Chelkov, G. A.; Chelstowska, M. A.; Chen, C.; Chen, H.; Chen, S.; Chen, S.; Chen, X.; Chen, Y.; Cheng, H. C.; Cheng, H. J.; Cheng, Y.; Cheplakov, A.; Cheremushkina, E.; El Moursli, R. Cherkaoui; Chernyatin, V.; Cheu, E.; Chevalier, L.; Chiarella, V.; Chiarelli, G.; Chiodini, G.; Chisholm, A. S.; Chitan, A.; Chiu, Y. H.; Chizhov, M. V.; Choi, K.; Chomont, A. R.; Chouridou, S.; Chow, B. K. B.; Christodoulou, V.; Chromek-Burckhart, D.; Chudoba, J.; Chuinard, A. J.; Chwastowski, J. J.; Chytka, L.; Ciftci, A. K.; Cinca, D.; Cindro, V.; Cioara, I. A.; Ciocca, C.; Ciocio, A.; Cirotto, F.; Citron, Z. H.; Citterio, M.; Ciubancan, M.; Clark, A.; Clark, B. L.; Clark, M. R.; Clark, P. J.; Clarke, R. N.; Clement, C.; Coadou, Y.; Cobal, M.; Coccaro, A.; Cochran, J.; Colasurdo, L.; Cole, B.; Colijn, A. P.; Collot, J.; Colombo, T.; Muiño, P. Conde; Coniavitis, E.; Connell, S. H.; Connelly, I. A.; Consorti, V.; Constantinescu, S.; Conti, G.; Conventi, F.; Cooke, M.; Cooper, B. D.; Cooper-Sarkar, A. M.; Cormier, F.; Cormier, K. J. R.; Cornelissen, T.; Corradi, M.; Corriveau, F.; Cortes-Gonzalez, A.; Cortiana, G.; Costa, G.; Costa, M. J.; Costanzo, D.; Cottin, G.; Cowan, G.; Cox, B. E.; Cranmer, K.; Crawley, S. J.; Cree, G.; Crépé-Renaudin, S.; Crescioli, F.; Cribbs, W. A.; Ortuzar, M. Crispin; Cristinziani, M.; Croft, V.; Crosetti, G.; Cueto, A.; Donszelmann, T. Cuhadar; Cummings, J.; Curatolo, M.; Cúth, J.; Czirr, H.; Czodrowski, P.; D'amen, G.; D'Auria, S.; D'Onofrio, M.; Da Cunha Sargedas De Sousa, M. J.; Da Via, C.; Dabrowski, W.; Dado, T.; Dai, T.; Dale, O.; Dallaire, F.; Dallapiccola, C.; Dam, M.; Dandoy, J. R.; Dang, N. P.; Daniells, A. C.; Dann, N. S.; Danninger, M.; Hoffmann, M. Dano; Dao, V.; Darbo, G.; Darmora, S.; Dassoulas, J.; Dattagupta, A.; Davey, W.; David, C.; Davidek, T.; Davies, M.; Davison, P.; Dawe, E.; Dawson, I.; De, K.; de Asmundis, R.; De Benedetti, A.; De Castro, S.; De Cecco, S.; De Groot, N.; de Jong, P.; De la Torre, H.; De Lorenzi, F.; De Maria, A.; De Pedis, D.; De Salvo, A.; De Sanctis, U.; De Santo, A.; De Vivie De Regie, J. B.; Dearnaley, W. J.; Debbe, R.; Debenedetti, C.; Dedovich, D. V.; Dehghanian, N.; Deigaard, I.; Del Gaudio, M.; Del Peso, J.; Del Prete, T.; Delgove, D.; Deliot, F.; Delitzsch, C. M.; Dell'Acqua, A.; Dell'Asta, L.; Dell'Orso, M.; Pietra, M. Della; della Volpe, D.; Delmastro, M.; Delsart, P. A.; DeMarco, D. A.; Demers, S.; Demichev, M.; Demilly, A.; Denisov, S. P.; Denysiuk, D.; Derendarz, D.; Derkaoui, J. E.; Derue, F.; Dervan, P.; Desch, K.; Deterre, C.; Dette, K.; Deviveiros, P. O.; Dewhurst, A.; Dhaliwal, S.; Di Ciaccio, A.; Di Ciaccio, L.; Di Clemente, W. K.; Di Donato, C.; Di Girolamo, A.; Di Girolamo, B.; Di Micco, B.; Di Nardo, R.; Di Petrillo, K. F.; Di Simone, A.; Di Sipio, R.; Di Valentino, D.; Diaconu, C.; Diamond, M.; Dias, F. A.; Diaz, M. A.; Diehl, E. B.; Dietrich, J.; Cornell, S. Díez; Dimitrievska, A.; Dingfelder, J.; Dita, P.; Dita, S.; Dittus, F.; Djama, F.; Djobava, T.; Djuvsland, J. I.; do Vale, M. A. B.; Dobos, D.; Dobre, M.; Doglioni, C.; Dolejsi, J.; Dolezal, Z.; Donadelli, M.; Donati, S.; Dondero, P.; Donini, J.; Dopke, J.; Doria, A.; Dova, M. T.; Doyle, A. T.; Drechsler, E.; Dris, M.; Du, Y.; Duarte-Campderros, J.; Duchovni, E.; Duckeck, G.; Ducu, O. A.; Duda, D.; Dudarev, A.; Dudder, A. Chr.; Duffield, E. M.; Duflot, L.; Dührssen, M.; Dumancic, M.; Duncan, A. K.; Dunford, M.; Yildiz, H. Duran; Düren, M.; Durglishvili, A.; Duschinger, D.; Dutta, B.; Dyndal, M.; Eckardt, C.; Ecker, K. M.; Edgar, R. C.; Edwards, N. C.; Eifert, T.; Eigen, G.; Einsweiler, K.; Ekelof, T.; El Kacimi, M.; Ellajosyula, V.; Ellert, M.; Elles, S.; Ellinghaus, F.; Elliot, A. A.; Ellis, N.; Elmsheuser, J.; Elsing, M.; Emeliyanov, D.; Enari, Y.; Endner, O. C.; Ennis, J. S.; Erdmann, J.; Ereditato, A.; Ernis, G.; Ernst, J.; Ernst, M.; Errede, S.; Ertel, E.; Escalier, M.; Esch, H.; Escobar, C.; Esposito, B.; Etienvre, A. I.; Etzion, E.; Evans, H.; Ezhilov, A.; Fabbri, F.; Fabbri, L.; Facini, G.; Fakhrutdinov, R. M.; Falciano, S.; Falla, R. J.; Faltova, J.; Fang, Y.; Fanti, M.; Farbin, A.; Farilla, A.; Farina, C.; Farina, E. M.; Farooque, T.; Farrell, S.; Farrington, S. M.; Farthouat, P.; Fassi, F.; Fassnacht, P.; Fassouliotis, D.; Giannelli, M. Faucci; Favareto, A.; Fawcett, W. J.; Fayard, L.; Fedin, O. L.; Fedorko, W.; Feigl, S.; Feligioni, L.; Feng, C.; Feng, E. J.; Feng, H.; Fenyuk, A. B.; Feremenga, L.; Martinez, P. Fernandez; Perez, S. Fernandez; Ferrando, J.; Ferrari, A.; Ferrari, P.; Ferrari, R.; de Lima, D. E. Ferreira; Ferrer, A.; Ferrere, D.; Ferretti, C.; Fiedler, F.; Filipčič, A.; Filipuzzi, M.; Filthaut, F.; Fincke-Keeler, M.; Finelli, K. D.; Fiolhais, M. C. N.; Fiorini, L.; Fischer, A.; Fischer, C.; Fischer, J.; Fisher, W. C.; Flaschel, N.; Fleck, I.; Fleischmann, P.; Fletcher, G. T.; Fletcher, R. R. M.; Flick, T.; Flierl, B. M.; Castillo, L. R. Flores; Flowerdew, M. J.; Forcolin, G. T.; Formica, A.; Forti, A.; Foster, A. G.; Fournier, D.; Fox, H.; Fracchia, S.; Francavilla, P.; Franchini, M.; Francis, D.; Franconi, L.; Franklin, M.; Frate, M.; Fraternali, M.; Freeborn, D.; Fressard-Batraneanu, S. M.; Friedrich, F.; Froidevaux, D.; Frost, J. A.; Fukunaga, C.; Torregrosa, E. Fullana; Fusayasu, T.; Fuster, J.; Gabaldon, C.; Gabizon, O.; Gabrielli, A.; Gabrielli, A.; Gach, G. P.; Gadatsch, S.; Gagliardi, G.; Gagnon, L. G.; Gagnon, P.; Galea, C.; Galhardo, B.; Gallas, E. J.; Gallop, B. J.; Gallus, P.; Galster, G.; Gan, K. K.; Ganguly, S.; Gao, J.; Gao, Y.; Gao, Y. S.; Walls, F. M. Garay; García, C.; Navarro, J. E. García; Garcia-Sciveres, M.; Gardner, R. W.; Garelli, N.; Garonne, V.; Bravo, A. Gascon; Gasnikova, K.; Gatti, C.; Gaudiello, A.; Gaudio, G.; Gauthier, L.; Gavrilenko, I. L.; Gay, C.; Gaycken, G.; Gazis, E. N.; Gecse, Z.; Gee, C. N. P.; Geich-Gimbel, Ch.; Geisen, M.; Geisler, M. P.; Gellerstedt, K.; Gemme, C.; Genest, M. H.; Geng, C.; Gentile, S.; Gentsos, C.; George, S.; Gerbaudo, D.; Gershon, A.; Ghasemi, S.; Ghneimat, M.; Giacobbe, B.; Giagu, S.; Giannetti, P.; Gibson, S. M.; Gignac, M.; Gilchriese, M.; Gillam, T. P. S.; Gillberg, D.; Gilles, G.; Gingrich, D. M.; Giokaris, N.; Giordani, M. P.; Giorgi, F. M.; Giraud, P. F.; Giromini, P.; Giugni, D.; Giuli, F.; Giuliani, C.; Giulini, M.; Gjelsten, B. K.; Gkaitatzis, S.; Gkialas, I.; Gkougkousis, E. L.; Gladilin, L. K.; Glasman, C.; Glatzer, J.; Glaysher, P. C. F.; Glazov, A.; Goblirsch-Kolb, M.; Godlewski, J.; Goldfarb, S.; Golling, T.; Golubkov, D.; Gomes, A.; Gonçalo, R.; Gama, R. 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B.; Queitsch-Maitland, M.; Quilty, D.; Raddum, S.; Radeka, V.; Radescu, V.; Radhakrishnan, S. K.; Radloff, P.; Rados, P.; Ragusa, F.; Rahal, G.; Raine, J. A.; Rajagopalan, S.; Rammensee, M.; Rangel-Smith, C.; Ratti, M. G.; Rauch, D. M.; Rauscher, F.; Rave, S.; Ravenscroft, T.; Ravinovich, I.; Raymond, M.; Read, A. L.; Readioff, N. P.; Reale, M.; Rebuzzi, D. M.; Redelbach, A.; Redlinger, G.; Reece, R.; Reed, R. G.; Reeves, K.; Rehnisch, L.; Reichert, J.; Reiss, A.; Rembser, C.; Ren, H.; Rescigno, M.; Resconi, S.; Resseguie, E. D.; Rezanova, O. L.; Reznicek, P.; Rezvani, R.; Richter, R.; Richter, S.; Richter-Was, E.; Ricken, O.; Ridel, M.; Rieck, P.; Riegel, C. J.; Rieger, J.; Rifki, O.; Rijssenbeek, M.; Rimoldi, A.; Rimoldi, M.; Rinaldi, L.; Ristić, B.; Ritsch, E.; Riu, I.; Rizatdinova, F.; Rizvi, E.; Rizzi, C.; Roberts, R. T.; Robertson, S. H.; Robichaud-Veronneau, A.; Robinson, D.; Robinson, J. E. M.; Robson, A.; Roda, C.; Rodina, Y.; Perez, A. Rodriguez; Rodriguez, D. 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C.; Yasu, Y.; Yatsenko, E.; Wong, K. H. Yau; Ye, J.; Ye, S.; Yeletskikh, I.; Yildirim, E.; Yorita, K.; Yoshida, R.; Yoshihara, K.; Young, C.; Young, C. J. S.; Youssef, S.; Yu, D. R.; Yu, J.; Yu, J. M.; Yu, J.; Yuan, L.; Yuen, S. P. Y.; Yusuff, I.; Zabinski, B.; Zacharis, G.; Zaidan, R.; Zaitsev, A. M.; Zakharchuk, N.; Zalieckas, J.; Zaman, A.; Zambito, S.; Zanzi, D.; Zeitnitz, C.; Zeman, M.; Zemla, A.; Zeng, J. C.; Zeng, Q.; Zenin, O.; Ženiš, T.; Zerwas, D.; Zhang, D.; Zhang, F.; Zhang, G.; Zhang, H.; Zhang, J.; Zhang, L.; Zhang, L.; Zhang, M.; Zhang, R.; Zhang, R.; Zhang, X.; Zhang, Y.; Zhang, Z.; Zhao, X.; Zhao, Y.; Zhao, Z.; Zhemchugov, A.; Zhong, J.; Zhou, B.; Zhou, C.; Zhou, L.; Zhou, L.; Zhou, M.; Zhou, M.; Zhou, N.; Zhu, C. G.; Zhu, H.; Zhu, J.; Zhu, Y.; Zhuang, X.; Zhukov, K.; Zibell, A.; Zieminska, D.; Zimine, N. I.; Zimmermann, C.; Zimmermann, S.; Zinonos, Z.; Zinser, M.; Ziolkowski, M.; Živković, L.; Zobernig, G.; Zoccoli, A.; zur Nedden, M.; Zwalinski, L. Bibcode: 2017JHEP...04..124A Altcode: 2019arXiv190605310A To probe the W tb vertex structure, top-quark and W -boson polarisation observables are measured from t-channel single-top-quark events produced in proton-proton collisions at a centre-of-mass energy of 8 TeV. The dataset corresponds to an integrated luminosity of 20.2 fb-1, recorded with the ATLAS detector at the LHC. Selected events contain one isolated electron or muon, large missing transverse momentum and exactly two jets, with one of them identified as likely to contain a b-hadron. Stringent selection requirements are applied to discriminate t-channel single-top-quark events from background. The polarisation observables are extracted from asymmetries in angular distributions measured with respect to spin quantisation axes appropriately chosen for the top quark and the W boson. The asymmetry measurements are performed at parton level by correcting the observed angular distributions for detector effects and hadronisation after subtracting the background contributions. The measured top-quark and W -boson polarisation values are in agreement with the Standard Model predictions. Limits on the imaginary part of the anomalous coupling g R are also set from model-independent measurements. [Figure not available: see fulltext.] Title: 2017 FL1 Authors: Read, M. T.; Johnson, J. A.; Christensen, E. J.; Fuls, D. C.; Gibbs, A. R.; Grauer, A. D.; Kowalski, R. A.; Larson, S. M.; Leonard, G. J.; Matheny, R. G.; Seaman, R. L.; Shelly, F. C.; Schwartz, M.; Holvorcem, P. R.; McCarthy Obs, J. J.; Robson, M.; Moore, R.; Matthews, J.; Matthews, K.; Bosch, J. M.; Mantero, A.; Gibson, B.; Goggia, T.; Kahale, S.; Lowe, T.; Schultz, A.; Willman, M.; Chambers, K.; Chastel, S.; Denneau, L.; Flewelling, H.; Huber, M.; Lilly, E.; Magnier, E.; Wainscoat, R.; Waters, C.; Weryk, R.; Ryan, W. H.; Ryan, E. V.; Holmes, R.; Foglia, S.; Buzzi, L.; Linder, T.; Hudin, L.; Rowe, B. Bibcode: 2017MPEC....F...42R Altcode: No abstract at ADS Title: Evaluation of the Minifilament-Eruption Scenario for Solar Coronal Jets in Polar Coronal Holes Authors: Sterling, A. C.; Baikie, T. K.; Falconer, D. A.; Moore, R. L.; Savage, S. L. Bibcode: 2016AGUFMSH31B2574S Altcode: Solar coronal jets are suspected to result from magnetic reconnection low in the Sun's atmosphere. Sterling et al. (2015) looked at 20 jets in polar coronal holes, using X-ray images from the Hinode/X-Ray Telescope (XRT) and EUV images from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA). They suggested that each jet was driven by the eruption of twisted closed magnetic field carrying a small-scale filament, which they call a "minifilament", and that the jet was produced by reconnection of the erupting field with surrounding open field. In this study, we carry out a more extensive examination of polar coronal jets. From 280 hours of XRT polar coronal hole observations spread over two years (2014-2016), we identified 117 clearly-identifiable X-ray jet events. From the broader set, we selected 25 of the largest and brightest events for further study in AIA 171, 193, 211, and 304 Angstrom images. We find that at least the majority of the jets follow the minifilament-eruption scenario, although for some cases the evolution of the minifilament in the onset of its eruption is more complex then presented in the simplified schematic of Sterling et al. (2015). For all cases in which we could make a clear determination, the spire of the X-ray jet drifted laterally away from the jet-base-edge bright point; this spire drift away from the bright point is consistent with expectations of the minifilament-eruption scenario for coronal-jet production. This work was supported with funding from the NASA/MSFC Hinode Project Office, and from the NASA HGI program. Title: Solar Coronal Jets in Active Regions Authors: Sterling, A. C.; Moore, R. L.; Martinez, F.; Falconer, D. A. Bibcode: 2016AGUFMSH43E..06S Altcode: Solar coronal jets are common in both coronal holes and in active regions. Recently, Sterling et al. (2015, Nature 523, 437), using data from Hinode/XRT and SDO/AIA, found that coronal jets originating in polar coronal holes result from the eruption of small-scale filaments (minifilaments). The jet bright point (JBP) seen in X-rays and hotter EUV channels off to one side of the base of the jet's spire develops at the location where the minifilament erupts, consistent with the JBPs being miniature versions of typical solar flares that occur in the wake of large-scale filament eruptions. Here we consider whether active region coronal jets also result from the same minifilament-eruption mechanism, or whether they instead result from a different process, such as emerging flux. Here we present observations of NOAA active region 12259, over 13-20 Jan 2015, using observations from Hinode/XRT, and from SDO/AIA and HMI. We focused on 13 standout jets that we identified from an initial survey of the XRT X-ray images, and we found many more jets in the AIA data set, which have higher cadence and more continuous coverage than our XRT data. All 13 jets originated from identifiable magnetic neutral lines; we further found magnetic flux cancelation to be occurring at essentially all of these neutral lines. At least 6 of those 13 jets were homologous, developing with similar morphology from nearly the same location, and in fact there were many more jets in the homologous sequence apparent in the higher-fidelity AIA data. Each of these homologous jets was consistent with minifilament-like ejections at the start of the jets. Other jets displayed a variety of morphologies, at least some of which were consistent with minifilament eruptions. For other jets however we have not yet clearly deciphered the driving mechanism. Our overall conclusions are similar to those of our earlier study of active region jets (Sterling et al. 2016, ApJ, 821, 100), where we found: some jets clearly to result from mini-filament eruptions; it was difficult to disentangle the mechanism of some other jets; and all of the jets originated from magnetic neutral lines, most of which were undergoing flux cancelation. This work was supported by funding from NASA/HGI, from the Hinode project, and (for FM) from the NASA/MSFC Research Experience for Undergraduates (REU) program. Title: Sunspot Coronal Fan Loops: Location, Closure, and Heating Authors: Heerikhuisen, J.; Ruiz, S.; Tiwari, S. K.; Moore, R. L.; Winebarger, A. R. Bibcode: 2016AGUFMSH31B2578H Altcode: We define sunspot coronal fan loops to be structures that are bright in Fe IX/X 171Å images, have fan-like appearance, and have a foot in a sunspot. The exact location in aggregate within the sunspot in which the coronal fan loops are rooted has not previously been studied. Through umbra-edge and penumbra-edge maps and potential field extrapolations we show that fan loops are commonly found in the center of the umbra in single sunspot active regions, although they can also be located in the outer umbra or the penumbra. In bipolar active regions, a fan loop can be rooted in the center of the umbra at one footpoint as long as the other footpoint is located in a convective region e.g., in a plage or penumbra. Furthermore, the extrapolations illustrate that it is unlikely for fan loops to be open, which disagrees with the previously thought idea that fan loops occur along open magnetic field lines hosting a slow solar wind. We infer that any coronal field loop having one foot in a sunspot umbra (with no fan loops in it) has its other foot either in another umbra or in weak magnetic flux. Title: Flux Cancellation Leading to Solar Filament Eruptions Authors: Popescu, R. M.; Panesar, N. K.; Sterling, A. C.; Moore, R. L. Bibcode: 2016AGUFMSH31B2572P Altcode: Solar filaments are strands of relatively cool, dense plasma magnetically suspended in the lower density hotter solar corona. They trace magnetic polarity inversion lines (PILs) in the photosphere below, and are supported against gravity at heights of up to 100 Mm above the chromosphere by the magnetic field in and around them. This field erupts when it is rendered unstable by either magnetic flux cancellation or emergence at or near the PIL. We have studied the evolution of photospheric magnetic flux leading to ten observed filament eruptions. Specifically, we look for gradual magnetic changes in the neighborhood of the PIL prior to and during eruption. We use Extreme Ultraviolet (EUV) images from the Atmospheric Imaging Assembly (AIA), and magnetograms from the Helioseismic and Magnetic Imager (HMI), both onboard the Solar Dynamics Observatory (SDO), to study filament eruptions and their photospheric magnetic fields. We examine whether flux cancellation or/and emergence leads to filament eruptions and find that continuous flux cancellation was present at the PIL for many hours prior to each eruption. We present two events in detail and find the following: (a) the pre-eruption filament-holding core field is highly sheared and appears in the shape of a sigmoid above the PIL; (b) at the start of the eruption the opposite arms of the sigmoid reconnect in the middle above the site of (tether-cutting) flux cancellation at the PIL; (c) the filaments first show a slow-rise, followed by a fast-rise as they erupt. We conclude that these two filament eruptions result from flux cancellation in the middle of the sheared field and are in agreement with the standard model for a CME/flare filament eruption from a closed bipolar magnetic field [flux cancellation (van Ballegooijen and Martens 1989 and Moore and Roumelrotis 1992) and runaway tether-cutting (Moore et. al 2001)]. Title: A New Method to Quantify and Reduce the net Projection Error in Whole-solar-active-region Parameters Measured from Vector Magnetograms Authors: Falconer, David A.; Tiwari, Sanjiv K.; Moore, Ronald L.; Khazanov, Igor Bibcode: 2016ApJ...833L..31F Altcode: 2016arXiv161201948F Projection errors limit the use of vector magnetograms of active regions (ARs) far from the disk center. In this Letter, for ARs observed up to 60° from the disk center, we demonstrate a method for measuring and reducing the projection error in the magnitude of any whole-AR parameter that is derived from a vector magnetogram that has been deprojected to the disk center. The method assumes that the center-to-limb curve of the average of the parameter’s absolute values, measured from the disk passage of a large number of ARs and normalized to each AR’s absolute value of the parameter at central meridian, gives the average fractional projection error at each radial distance from the disk center. To demonstrate the method, we use a large set of large-flux ARs and apply the method to a whole-AR parameter that is among the simplest to measure: whole-AR magnetic flux. We measure 30,845 SDO/Helioseismic and Magnetic Imager vector magnetograms covering the disk passage of 272 large-flux ARs, each having whole-AR flux >1022 Mx. We obtain the center-to-limb radial-distance run of the average projection error in measured whole-AR flux from a Chebyshev fit to the radial-distance plot of the 30,845 normalized measured values. The average projection error in the measured whole-AR flux of an AR at a given radial distance is removed by multiplying the measured flux by the correction factor given by the fit. The correction is important for both the study of the evolution of ARs and for improving the accuracy of forecasts of an AR’s major flare/coronal mass ejection productivity. Title: Coronal Jets from Minifilament Eruptions in Active Regions Authors: Sterling, A. C.; Martinez, F.; Falconer, D. A.; Moore, R. L. Bibcode: 2016AGUFMSH31B2567S Altcode: Solar coronal jets are transient (frequently of lifetime 10 min) features that shoot out from near the solar surface, become much longer than their width, and occur in all solar regions, including coronal holes, quiet Sun, and active regions (e.g., Shimojo et al. 1996, Certain et al. 2007). Sterling et al. (2015) and other studies found that in coronal holes and in quiet Sun the jets result when small-scale filaments, called ``minifilaments,'' erupt onto nearby open or high-reaching field lines. Additional studies found that coronal-jet-onset locations (and hence presumably the minifilament-eruption-onset locations) coincided with locations of magnetic-flux cancellation. For active region (AR) jets however the situation is less clear. Sterling et al. (2016) studied jets in one active region over a 24-hour period; they found that some AR jets indeed resulted from minifilament eruptions, usually originating from locations of episodes of magnetic-flux cancelation. In some cases however they could not determine whether flux was emerging or canceling at the polarity inversion line from which the minifilament erupted; and for other jets of that region minifilaments were not conclusively apparent prior to jet occurrence. Here we further study AR jets, by observing them in a single AR over a one-week period, using X-ray images from Hinode/XRT and EUV/UV images from SDO/AIA, and line-of-sight magnetograms and white-light intensity-grams from SDO/HMI. We initially identified 13 prominent jets in the XRT data, and examined corresponding AIA and HMI data. For at least several of the jets, our findings are consistent with the jets resulting from minifilament eruptions, and originating from sights of magnetic-field cancelation. Thus our findings support that, at least in many cases, AR coronal jets result from the same physical processes that produce coronal jets in quiet-Sun and coronal-hole regions. FM was supportedby the Research Experience for Undergraduates (REU) program at NASA/MSFC and the University of Alabama, Huntsville. Additional support was from the NASA HGI program and the Hinode project. Title: Plumes in Solar Coronal Holes: Magnetic Flux Content and Luminosity Authors: Paiste, J. H.; Tiwari, S. K.; Moore, R. L.; Winebarger, A. R. Bibcode: 2016AGUFMSH31B2573P Altcode: On-disc coronal hole plumes, formation and disappearance of which might have implications on heating of coronal loops, have drawn attention from several researchers recently. Raouafi et al. (2014) proposed that plumes form when magnetic reconnection at their footpoints occurs. Other observations, e.g. Wang et al. (2016), have shown that plumes form when magnetic flux at their feet in the photosphere converges and they disappear when the magnetic flux at their feet diverges. In this work, we take a quantitative look at this hypothesis, and find that the luminosity of plumes in 171 Å Fe IX/X emission broadly peaks in step with the plume-base flux content of unipolar magnetic field stronger than 200 Gauss. Flux convergence/divergence seems to help flux grow/decay at the plume base leading to brighter/dimmer intensity in AIA 171 channel. Title: Magnetic Flux Cancelation as the Trigger of Solar Quiet-region Coronal Jets Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L.; Chakrapani, Prithi Bibcode: 2016ApJ...832L...7P Altcode: 2016arXiv161008540P We report observations of 10 random on-disk solar quiet-region coronal jets found in high-resolution extreme ultraviolet (EUV) images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly and having good coverage in magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). Recent studies show that coronal jets are driven by the eruption of a small-scale filament (called a minifilament). However, the trigger of these eruptions is still unknown. In the present study, we address the question: what leads to the jet-driving minifilament eruptions? The EUV observations show that there is a cool-transition-region-plasma minifilament present prior to each jet event and the minifilament eruption drives the jet. By examining pre-jet evolutionary changes in the line of sight photospheric magnetic field, we observe that each pre-jet minifilament resides over the neutral line between majority-polarity and minority-polarity patches of magnetic flux. In each of the 10 cases, the opposite-polarity patches approach and merge with each other (flux reduction between 21% and 57%). After several hours, continuous flux cancelation at the neutral line apparently destabilizes the field holding the cool-plasma minifilament to erupt and undergo internal reconnection, and external reconnection with the surrounding coronal field. The external reconnection opens the minifilament field allowing the minifilament material to escape outward, forming part of the jet spire. Thus, we found that each of the 10 jets resulted from eruption of a minifilament following flux cancelation at the neutral line under the minifilament. These observations establish that magnetic flux cancelation is usually the trigger of quiet-region coronal jet eruptions. Title: Babcock Redux: An Amendment of Babcock's Schematic of the Sun's Magnetic Cycle Authors: Moore, Ronald L.; Cirtain, Jonathan W.; Sterling, Alphonse C. Bibcode: 2016usc..confE...5M Altcode: 2016arXiv160605371M We amend Babcock's original scenario for the global dynamo process that sustains the Sun's 22-year magnetic cycle. The amended scenario fits post-Babcock observed features of the magnetic activity cycle and convection zone, and is based on ideas of Spruit & Roberts (1983) about magnetic flux tubes in the convection zone. A sequence of four schematic cartoons lays out the proposed evolution of the global configuration of the magnetic field above, in, and at the bottom of the convection zone through sunspot Cycle 23 and into Cycle 24. Three key elements of the amended scenario are: (1) as the net following-polarity magnetic field from the sunspot-region -loop fields of an ongoing sunspot cycle is swept poleward to cancel and replace the opposite-polarity polar-cap field from the previous sunspot cycle, it remains connected to the ongoing sunspot cycle's toroidal source-field band at the bottom of the convection zone; (2) topological pumping by the convection zone's free convection keeps the horizontal extent of the poleward-migrating following-polarity field pushed to the bottom, forcing it to gradually cancel and replace old horizontal field below it that connects the ongoing-cycle source-field band to the previous-cycle polar-cap field; (3) in each polar hemisphere, by continually shearing the poloidal component of the settling new horizontal field, the latitudinal differential rotation low in the convection zone generates the next-cycle source-field band poleward of the ongoing-cycle band. The amended scenario is a more-plausible version of Babcock's scenario, and its viability can be explored by appropriate kinematic flux-transport solar-dynamo simulations. A paper of the above title and authors, giving a full description of the solar dynamo scenario of this abstract, is available at http://arxiv.org/abs/1606.05371. This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program and the Hinode Project. Title: A Microfilament-eruption Mechanism for Solar Spicules Authors: Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2016ApJ...828L...9S Altcode: 2016arXiv161200430S Recent investigations indicate that solar coronal jets result from eruptions of small-scale chromospheric filaments, called minifilaments; that is, the jets are produced by scaled-down versions of typical-sized filament eruptions. We consider whether solar spicules might in turn be scaled-down versions of coronal jets, being driven by eruptions of microfilaments. Assuming a microfilament's size is about a spicule's width (∼300 km), the estimated occurrence number plotted against the estimated size of erupting filaments, minifilaments, and microfilaments approximately follows a power-law distribution (based on counts of coronal mass ejections, coronal jets, and spicules), suggesting that many or most spicules could result from microfilament eruptions. Observed spicule-base Ca II brightenings plausibly result from such microfilament eruptions. By analogy with coronal jets, microfilament eruptions might produce spicules with many of their observed characteristics, including smooth rise profiles, twisting motions, and EUV counterparts. The postulated microfilament eruptions are presumably eruptions of twisted-core micro-magnetic bipoles that are ∼1.″0 wide. These explosive bipoles might be built and destabilized by merging and cancelation of approximately a few to 100 G magnetic-flux elements of size ≲ 0\buildrel{\prime\prime}\over{.} 5{--}1\buildrel{\prime\prime}\over{.} 0. If, however, spicules are relatively more numerous than indicated by our extrapolated distribution, then only a fraction of spicules might result from this proposed mechanism. Title: 2016 SH1 Authors: Bacci, P.; Tesi, L.; Fagioli, G.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Foglia, S.; Galli, G.; Buzzi, L.; Tichy, M.; Ticha, J.; Sarneczky, K.; Sicoli, P.; Testa, A.; Pettarin, E.; Piani, F.; Matheny, R. G.; Christensen, E. J.; Fuls, D. C.; Gibbs, A. R.; Grauer, A. D.; Johnson, J. A.; Kowalski, R. A.; Larson, S. M.; Leonard, G. J.; Seaman, R. L.; Shelly, F. C.; Durig, D. T.; Schwartz, M.; Holvorcem, P. R.; McCarthy Obs, J. J.; Polansky, M.; Moore, R.; Yapoujian, B.; Spencer, A.; Dupouy, P.; de Vanssay, J. B.; Dangl, G.; Mantero, A.; Birtwhistle, P.; Hudin, L.; Rankin, D.; Mickleburgh, A. Bibcode: 2016MPEC....S...51B Altcode: No abstract at ADS Title: Suppression of heating of coronal loops rooted in opposite polarity sunspot umbrae Authors: Tiwari, Sanjiv K.; Thalmann, Julia; Moore, Ronald; Panesar, Navdeep; Winebarger, Amy Bibcode: 2016shin.confE..61T Altcode: EUV observations of active region (AR) coronae reveal the presence of loops at different temperatures. To understand the mechanisms that result in hotter or cooler loops, we study a typical bipolar AR, near solar disk center, which has moderate overall magnetic twist and at least one fully developed sunspot of each polarity. From AIA 193 and 94 Å images we identify many clearly discernible coronal loops that connect plage or a sunspot of one polarity to an opposite-polarity plage region. The AIA 94 Å images show dim regions in the umbrae of the sunspots. To see which coronal loops are rooted in a dim umbral area, we performed a non-linear force-free field (NLFFF) modeling using photospheric vector magnetic field measurements obtained with the Heliosesmic Magnetic Imager (HMI) onboard SDO. The NLFFF model, validated by comparison of calculated model field lines with observed loops in AIA 193 and 94 Å, specifies the photospheric roots of the model field lines. Some model coronal magnetic field lines arch from the dim umbral area of the positive-polarity sunspot to the dim umbral area of a negative-polarity sunspot. Because these coronal loops are not visible in any of the coronal EUV and X-ray images of the AR, we conclude they are the coolest loops in the AR. This result suggests that the loops connecting opposite polarity umbrae are the least heated because the field in umbrae is so strong that the convective braiding of the field is strongly suppressed. Title: Homologous Jet-driven Coronal Mass Ejections from Solar Active Region 12192 Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2016ApJ...822L..23P Altcode: 2016arXiv160405770P We report observations of homologous coronal jets and their coronal mass ejections (CMEs) observed by instruments onboard the Solar Dynamics Observatory (SDO) and the Solar and Heliospheric Observatory (SOHO) spacecraft. The homologous jets originated from a location with emerging and canceling magnetic field at the southeastern edge of the giant active region (AR) of 2014 October, NOAA 12192. This AR produced in its interior many non-jet major flare eruptions (X- and M- class) that made no CME. During October 20 to 27, in contrast to the major flare eruptions in the interior, six of the homologous jets from the edge resulted in CMEs. Each jet-driven CME (∼200-300 km s-1) was slower-moving than most CMEs, with angular widths (20°-50°) comparable to that of the base of a coronal streamer straddling the AR and were of the “streamer-puff” variety, whereby the preexisting streamer was transiently inflated but not destroyed by the passage of the CME. Much of the transition-region-temperature plasma in the CME-producing jets escaped from the Sun, whereas relatively more of the transition-region plasma in non-CME-producing jets fell back to the solar surface. Also, the CME-producing jets tended to be faster and longer-lasting than the non-CME-producing jets. Our observations imply that each jet and CME resulted from reconnection opening of twisted field that erupted from the jet base and that the erupting field did not become a plasmoid as previously envisioned for streamer-puff CMEs, but instead the jet-guiding streamer-base loop was blown out by the loop’s twist from the reconnection. Title: A Series of Streamer-Puff CMEs Driven by Solar Homologous Jets from Active Region 12192 Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Moore, Ronald L. Bibcode: 2016SPD....47.0622P Altcode: We investigate characteristics of solar coronal jets that originated from active region NOAA 12192 and produced coronal mass ejections (CMEs). This active region produced many non-jet major flare eruptions (X and M class) that made no CME. A multitude of jets occurred from the southeast edge of the active region, and in contrast to the major-flare eruptions in the core, six of these jets resulted in CMEs. Our jet observations are from multiple SDO/AIA EUV channels, including 304, 171 and 193Å, and CME observations are taken from SOHO/LASCO C2 coronograph. Each jet-driven CME was relatively slow-moving (~200 - 300 km s-1) compared to most CMEs; had angular width (20° - 50°) comparable to that of the streamer base; and was of the “streamer-puff” variety, whereby a preexisting streamer was transiently inflated but not removed (blown out) by the passage of the CME. Much of the chromospheric-temperature plasma of the jets producing the CMEs escaped from the Sun, whereas relatively more of the chromospheric plasma in the non-CME-producing jets fell back to the solar surface. We also found that the CME-producing jets tended to be faster in speed and longer in duration than the non-CME-producing jets. We expect that the jets result from eruptions of minifilaments (Sterling et al. 2015). We further propose that the CMEs are driven by magnetic twist injected into streamer-base coronal loops when erupting-twisted-minifilament field reconnects with the ambient field at the foot of those loops. This research was supported by funding from NASA's LWS program. Title: Analysis of an Anemone-Type Eruption in an On-Disk Coronal Hole Authors: Adams, Mitzi; Tennant, Allyn F.; Alexander, Caroline E.; Sterling, Alphonse C.; Moore, Ronald L.; Woolley, Robert Bibcode: 2016SPD....4740701A Altcode: We report on an eruption seen in a very small coronal hole (about 120'' across), beginning at approximately 19:00 UT on March 3, 2016. The event was initially observed by an amateur astronomer (RW) in an H-alpha movie from the Global Oscillation Network Group (GONG); the eruption attracted the attention of the observer because there was no nearby active region. To examine the region in detail, we use data from the Solar Dynamics Observatory (SDO), provided by the Atmospheric Imaging Assembly (AIA) in wavelengths 193 Å, 304 Å, and 94 Å, and the Helioseismic and Magnetic Imager (HMI). Data analysis and calibration activities such as scaling, rotation so that north is up, and removal of solar rotation are accomplished with SunPy. The eruption in low-cadence HMI data begins with the appearance of a bipole in the location of the coronal hole, followed by (apparent) expansion outwards when the intensity of the AIA wavelengths brighten; as the event proceeds, the coronal hole disappears. From high-cadence data, we will present results on the magnetic evolution of this structure, how it is related to intensity brightenings seen in the various SDO/AIA wavelengths, and how this event compares with the standard-anemone picture. Title: Minifilament Eruptions that Drive Coronal Jets in a Solar Active Region Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David; Panesar, Navdeep; Akiyama, Sachiko; Yashiro, Seiji; Gopalswamy, Nat Bibcode: 2016SPD....47.0334S Altcode: Solar coronal jets are common in both coronal holes and in active regions. Recently, Sterling et al. (2015), using data from Hinode/XRT and SDO/AIA, found that coronal jets originating in polar coronal holes result from the eruption of small-scale filaments (minifilaments). The jet bright point (JBP) seen in X-rays and hotter EUV channels off to one side of the base of the jet's spire develops at the location where the minifilament erupts, consistent with the JBPs being miniature versions of typical solar flares that occur in the wake of large-scale filament eruptions. Here we consider whether active region coronal jets also result from the same minifilament-eruption mechanism, or whether they instead result from a different mechanism, such as the hitherto popular ``emerging flux'' model for jets. We present observations of an on-disk active region that produced numerous jets on 2012 June 30, using data from SDO/AIA and HMI, and from GOES/SXI. We find that several of these active region jets also originate with eruptions of miniature filaments (size scale ~20'') emanating from small-scale magnetic neutral lines of the region. This demonstrates that active region coronal jets are indeed frequently driven by minifilament eruptions. Other jets from the active region were also consistent with their drivers being minifilament eruptions, but we could not confirm this because the onsets of those jets were hidden from our view. This work was supported by funding from NASA/LWS, NASA/HGI, and Hinode. Title: Hi-C Observations of Sunspot Penumbral Bright Dots Authors: Alpert, Shane E.; Tiwari, Sanjiv K.; Moore, Ronald L.; Winebarger, Amy R.; Savage, Sabrina L. Bibcode: 2016ApJ...822...35A Altcode: 2016arXiv160304968A We report observations of bright dots (BDs) in a sunspot penumbra using High Resolution Coronal Imager (Hi-C) data in 193 Å and examine their sizes, lifetimes, speeds, and intensities. The sizes of the BDs are on the order of 1″ and are therefore hard to identify in the Atmospheric Imaging Assembly (AIA) 193 Å images, which have a 1.″2 spatial resolution, but become readily apparent with Hi-C's spatial resolution, which is five times better. We supplement Hi-C data with data from AIA's 193 Å passband to see the complete lifetime of the BDs that appeared before and/or lasted longer than Hi-C's three-minute observation period. Most Hi-C BDs show clear lateral movement along penumbral striations, either toward or away from the sunspot umbra. Single BDs often interact with other BDs, combining to fade away or brighten. The BDs that do not interact with other BDs tend to have smaller displacements. These BDs are about as numerous but move slower on average than Interface Region Imaging Spectrograph (IRIS) BDs, which was recently reported by Tian et al., and the sizes and lifetimes are on the higher end of the distribution of IRIS BDs. Using additional AIA passbands, we compare the light curves of the BDs to test whether the Hi-C BDs have transition region (TR) temperatures like those of the IRIS BDs. The light curves of most Hi-C BDs peak together in different AIA channels, indicating that their temperatures are likely in the range of the cooler TR (1-4 × 105 K). Title: Suppression of heating of coronal loops rooted in opposite polarity sunspot umbrae Authors: Tiwari, Sanjiv K.; Thalmann, Julia K.; Moore, Ronald L.; Panesar, Navdeep; Winebarger, Amy R. Bibcode: 2016SPD....47.0336T Altcode: EUV observations of active region (AR) coronae reveal the presence of loops at different temperatures. To understand the mechanisms that result in hotter or cooler loops, we study a typical bipolar AR, near solar disk center, which has moderate overall magnetic twist and at least one fully developed sunspot of each polarity. From AIA 193 and 94 A images we identify many clearly discernible coronal loops that connect plage or a sunspot of one polarity to an opposite-polarity plage region. The AIA 94 A images show dim regions in the umbrae of the spots. To see which coronal loops are rooted in a dim umbral area, we performed a non-linear force-free field (NLFFF) modeling using photospheric vector magnetic field measurements obtained with the HMI onboard SDO. After validation of the NLFFF model by comparison of calculated model field lines and observed loops in AIA 193 and 94, we specify the photospheric roots of the model field lines. The model field then shows the coronal magnetic loops that arch from the dim umbral areas of the opposite polarity sunspots. Because these coronal loops are not visible in any of the coronal EUV and X-ray images of the AR, we conclude they are the coolest loops in the AR. This result suggests that the loops connecting opposite polarity umbrae are the least heated because the field in umbrae is so strong that the convective braiding of the field is strongly suppressed.We hypothesize that the convective freedom at the feet of a coronal loop, together with the strength of the field in the body of the loop, determines the strength of the heating. In particular, we expect the hottest coronal loops to have one foot in an umbra and the other foot in opposite-polarity penumbra or plage (coronal moss), the areas of strong field in which convection is not as strongly suppressed as in umbra. Many transient, outstandingly bright, loops in the AIA 94 movie of the AR do have this expected rooting pattern. We will also present another example of AR in which we find a similar rooting pattern of coronal loops. Title: Minifilament Eruptions that Drive Coronal Jets in a Solar Active Region Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Panesar, Navdeep K.; Akiyama, Sachiko; Yashiro, Seiji; Gopalswamy, Nat Bibcode: 2016ApJ...821..100S Altcode: We present observations of eruptive events in an active region adjacent to an on-disk coronal hole on 2012 June 30, primarily using data from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), SDO/Helioseismic and Magnetic Imager (HMI), and STEREO-B. One eruption is of a large-scale (∼100″) filament that is typical of other eruptions, showing slow-rise onset followed by a faster-rise motion starting as flare emissions begin. It also shows an “EUV crinkle” emission pattern, resulting from magnetic reconnections between the exploding filament-carrying field and surrounding field. Many EUV jets, some of which are surges, sprays and/or X-ray jets, also occur in localized areas of the active region. We examine in detail two relatively energetic ones, accompanied by GOES M1 and C1 flares, and a weaker one without a GOES signature. All three jets resulted from small-scale (∼20″) filament eruptions consistent with a slow rise followed by a fast rise occurring with flare-like jet-bright-point brightenings. The two more-energetic jets showed crinkle patters, but the third jet did not, perhaps due to its weakness. Thus all three jets were consistent with formation via erupting minifilaments, analogous to large-scale filament eruptions and to X-ray jets in polar coronal holes. Several other energetic jets occurred in a nearby portion of the active region; while their behavior was also consistent with their source being minifilament eruptions, we could not confirm this because their onsets were hidden from our view. Magnetic flux cancelation and emergence are candidates for having triggered the minifilament eruptions. Title: Transition-region/Coronal Signatures and Magnetic Setting of Sunspot Penumbral Jets: Hinode (SOT/FG), Hi-C, and SDO/AIA Observations Authors: Tiwari, Sanjiv K.; Moore, Ronald L.; Winebarger, Amy R.; Alpert, Shane E. Bibcode: 2016ApJ...816...92T Altcode: 2015arXiv151107900T Penumbral microjets (PJs) are transient narrow bright features in the chromosphere of sunspot penumbrae, first characterized by Katsukawa et al. using the Ca II H-line filter on Hinode's Solar Optical Telescope (SOT). It was proposed that the PJs form as a result of reconnection between two magnetic components of penumbrae (spines and interspines), and that they could contribute to the transition region (TR) and coronal heating above sunspot penumbrae. We propose a modified picture of formation of PJs based on recent results on the internal structure of sunspot penumbral filaments. Using data of a sunspot from Hinode/SOT, High Resolution Coronal Imager, and different passbands of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, we examine whether PJs have signatures in the TR and corona. We find hardly any discernible signature of normal PJs in any AIA passbands, except for a few of them showing up in the 1600 Å images. However, we discovered exceptionally stronger jets with similar lifetimes but bigger sizes (up to 600 km wide) occurring repeatedly in a few locations in the penumbra, where evidence of patches of opposite-polarity fields in the tails of some penumbral filaments is seen in Stokes-V images. These tail PJs do display signatures in the TR. Whether they have any coronal-temperature plasma is unclear. We infer that none of the PJs, including the tail PJs, directly heat the corona in active regions significantly, but any penumbral jet might drive some coronal heating indirectly via the generation of Alfvén waves and/or braiding of the coronal field. Title: Probing Solar Eruption by Tracking Magnetic Cavities and Filaments Authors: Sterling, A. C.; Johnson, J. R.; Moore, R. L.; Gibson, S. E. Bibcode: 2015AGUFMSH53B2489S Altcode: A solar eruption is a tremendous explosion on the Sun that happens when energy stored in twisted (or distorted) magnetic fields is suddenly released. When this field is viewed along the axis of the twist in projection at the limb, e.g. in EUV or white-light coronal images, the outer portions of the pre-eruption magnetic structure sometimes appears as a region of weaker emission, called a "coronal cavity," surrounded by a brighter envelope. Often a chromospheric filament resides near the base of the cavity and parallel to the cavity's central axis. Typically, both the cavity and filament move outward from the Sun at the start of an eruption of the magnetic field in which the cavity and filament reside. Studying properties the cavities and filaments just prior to and during eruption can help constrain models that attempt to explain why and how the eruptions occur. In this study, we examined six different at-limb solar eruptions using images from the Extreme Ultraviolet Imaging Telescope (EIT) aboard the Solar and Heliospheric Observatory (SOHO). For four of these eruptions we observed both cavities and filaments, while for the remaining two eruptions, one had only a cavity and the other only a filament visible in EIT images. All six eruptions were in comparatively-quiet solar regions, with one in the neighborhood of the polar crown. We measured the height and velocities of the cavities and filaments just prior to and during the start of their fast-eruption onsets. Our results support that the filament and cavity are integral parts of a single large-scale erupting magnetic-field system. We examined whether the eruption-onset heights were correlated with the expected magnetic field strengths of the eruption-source regions, but no clear correlation was found. We discuss possible reasons for this lack of correlation, and we also discuss future research directions. The research performed was supported by the National Science Foundation under Grant No. AGS-1460767; J.J. participated in the Research Experience for Undergraduates (REU) program, at NASA/MSFC. Additional support was from a grant from the NASA LWS program. Title: Evolution of Fine-scale Penumbral Magnetic Structure and Formation of Penumbral Jets Authors: Tiwari, S. K.; Moore, R. L.; Rempel, M.; Winebarger, A. R. Bibcode: 2015AGUFMSH13D2461T Altcode: Sunspot penumbra consists of spines (more vertical field) and penumbral filaments (interspines). Spines are outward extension of umbra. Penumbral filaments are recently found, both in observations and magnetohydrodynamic (MHD) simulations, to be magnetized stretched granule-like convective cells, with strong upflows near the head that continues along the central axis with weakening strength of the flow. Strong downflows are found at the tails of filaments and weak downflows along the sides of it. These lateral downflows often contain opposite polarity magnetic field to that of spines; most strongly near the heads of filaments. In spite of this advancement in understanding of small-scale structure of sunspot penumbra, how the filaments and spines evolve and interact remains uncertain. Penumbral jets, bright, transient features, seen in the chromosphere, are one of several dynamic events in sunspot penumbra. It has been proposed that these penumbral microjets result from component (acute angle) reconnection of the magnetic field in spines with that in interspines and could contribute to transition-region and coronal heating above sunspots. In a recent investigation, it was proposed that the jets form as a result of reconnection between the opposite polarity field at edges of filaments with spine field, and it was found that these jets do not significantly directly heat the corona above sunspots. We discuss how the proposed formation of penumbral jets is integral to the formation mechanism of penumbral filaments and spines, and may explain why penumbral jets are few and far between. We also point out that the generation of the penumbral jets could indirectly drive coronal heating via generation of MHD waves or braiding of the magnetic field. Title: Revised View of Solar X-Ray Jets Authors: Sterling, A. C.; Moore, R. L.; Falconer, D. A.; Adams, M. Bibcode: 2015AGUFMSH23D..04S Altcode: We investigate the onset of ~20 random X-ray jets observed by Hinode/XRT. Each jetwas near the limb in a polar coronal hole, and showed a ''bright point'' in anedge of the base of the jet, as is typical for previously-observed X-ray jets. Weexamined SDO/AIA EUV images of each of the jets over multiple AIA channels,including 304 Ang, which detects chromospheric emissions, and 171, 193, and 211 Ang,which detect cooler-coronal emissions. We find the jets to result from eruptionsof miniature (size <~10 arcsec) filaments from the bases of the jets. In manycases, much of the erupting-filament material forms a chromospheric-temperaturejet. In the cool-coronal channels, often the filament appears in absorption andthe hotter EUV component of the jet appears in emission. The jet bright point formsat the location from which the miniature filament erupts, analogous to theformation of a standard solar flare arcade via flare (``internal'') reconnection in the wake of the eruption of a typical larger-scale chromospheric filament. Thespire of the jet forms on open field lines that presumably have undergoneinterchange (''external'') reconnection with the erupting field that envelops andcarries the miniature filament. This is consistent with what we found for theonset of an on-disk coronal jet we examined in Adams et al. (2014), and theobservations of other workers. It is however not consistent with the basicversion of the ''emerging-flux model'' for X-ray jets. This work was supported byfunding from NASA/LWS, Hinode, and ISSI. Title: Exploring the properties of Solar Prominence Tornados Authors: Ahmad, E.; Panesar, N. K.; Sterling, A. C.; Moore, R. L. Bibcode: 2015AGUFMSH53B2485A Altcode: Solar prominences consist of relatively cool and dense plasma embedded in the hotter solar corona above the solar limb. They form along magnetic polarity inversion lines, and are magnetically supported against gravity at heights of up to ~100 Mm above the chromosphere. Often, parts of prominences visually resemble Earth-based tornados, with inverted-cone-shaped structures and internal motions suggestive of rotation. These "prominence tornados" clearly possess complex magnetic structure, but it is still not certain whether they actually rotate around a ''rotation'' axis, or instead just appear to do so because of composite internal material motions such as counter-streaming flows or lateral (i.e. transverse to the field) oscillations. Here we study the structure and dynamics of five randomly selected prominences, using extreme ultraviolet (EUV) 171 Å images obtained with high spatial and temporal resolution by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) spacecraft. All of the prominences resided in non-active-region locations, and displayed what appeared to be tornado-like rotational motions. Our set includes examples oriented both broadside and end-on to our line-of-sight. We created time-distance plots of horizontal slices at several different heights of each prominence, to study the horizontal plasma motions. We observed patterns of oscillations at various heights in each prominence, and we measured parameters of these oscillations. We find the oscillation time periods to range over ~50 - 90 min, with average amplitudes of ~6,000 km, and with average velocities of ~7 kms-1. We found similar values for prominences viewed either broadside or end-on; this observed isotropy of the lateral oscillatory motion suggests that the apparent oscillations result from actual rotational plasma motions and/or lateral oscillations of the magnetic field, rather than to counter-streaming flows. This research was supported by the National Science Foundation under Grant No. AGS-1460767; EA participated in the Research Experience for Undergraduates (REU) program, at NASA/MSFC. Additional support was from a grant from the NASA LWS program. Title: Magnetic Structure and Formation of On-disk Coronal Plumes Authors: Antonsson, S.; Tiwari, S. K.; Moore, R. L.; Winebarger, A. R. Bibcode: 2015AGUFMSH53B2486A Altcode: "Plumes" are feather-like features found on the solar disk, in the plage-like field concentrations of quiet regions. On-disk plumes are analogous to polar/coronal-hole plumes but have not been studied in detail in the past. We research their formation and characteristics, such as lifetime, intensity and magnetic setting at the feet. Atmospheric Imaging Assembly (AIA) images in the 171 Å filter and Helioseismic and Magnetic Imager (HMI) line-of-sight magnetograms, both from the Solar Dynamics Observatory (SDO), are analyzed with the IDL SolarSoftWare package and used to study the plumes. We find that on-disk plumes form at the places of converging magnetic fields, and disappear when those fields disperse. However, plumes disappear after nearby events, such as flares, or with the emergence of opposite polarity. The lifetime of each plume tends to be several days, although some appear and disappear within several hours. On-disk plumes outline magnetic fields close to the sun, allowing a better understanding of fine magnetic structures than before. Additionally, since plumes must be heated to around 600,000 K to be visible in 171 Å, their formation and characteristics could tell about how they, and therefore the corona, are heated. Title: A Series of Streamer-Puff CMEs Driven by Solar Homologous Jets Authors: Panesar, N. K.; Sterling, A. C.; Moore, R. L. Bibcode: 2015AGUFMSH54B..07P Altcode: Solar coronal jets are magnetically channeled narrow eruptions often observed in the solar atmosphere, typically in EUV and X-ray emission, and occurring in various solar environments including active regions and coronal holes. Their driving mechanism is still under discussion, but facts that we know about jets include: (a) they are ejected from or near sites of compact magnetic explosions (compact ejective solar flares), (b) they sometimes carry chromospheric material high into the corona along with coronal-temperature plasma, (c) the cool-material jet velocities can reach 100 km s-1 or more, and (d) some active-region jets produce coronal mass ejections (CMEs). Here we investigate characteristics of EUV jets that originated from active region NOAA 12192 and produced CMEs. This active region produced many non-jet major flare eruptions (X and M class) that made no CME. A multitude of jets also occurred in the region, and in contrast to the major-flare eruptions, seven of these jets resulted in CMEs. Our jet observations are from multiple SDO/AIA EUV channels, including 304, 171, 193 and 94 Å, and our CME observations are from SOHO/LASCO C2 images. Each jet-driven CME was relatively slow-moving; had angular width (30° - 70°) comparable to that of the streamer base; and was of the "streamer-puff" variety, whereby a preexisting streamer was transiently inflated but not removed (blown out) by the passage of the CME. Much of the chromospheric-temperature plasma of the jets producing the CMEs escaped from the Sun, whereas relatively more of the chromospheric plasma in the non-CME-producing jets fell back to the solar surface. We also found that the CME-producing jets tended to be faster in speed and longer in duration than the non-CME-producing jets. This research was supported by funding from NASA's LWS program. Title: Visibility of Hinode/XRT X-Ray Jets at AIA/EUV Wavelengths, a Temperature Indicator Authors: Sterling, A. C.; Bakucz Canario, D.; Moore, R. L.; Falconer, D. A. Bibcode: 2015AGUFMSH31B2415S Altcode: X-ray jets have been observed for years using data from the X-Ray Telescope (XRT) on the Hinode Satellite. Recently with the launch of the Solar Dynamics Observatory (SDO) it has been possible to observe solar jets over a range of EUV of wavelengths using the Atmospheric Imaging Assembly (AIA). In this study, we investigated the appearance of X-ray jets in AIA images at wavelengths of 304, 171, 193, 211, 131, 94, and 335 Å. We selected 20 random X-ray jets from XRT movies of the polar coronal holes and then examined AIA EUV images from the same locations and times to determine the visibility of the jets at the different EUV wavelengths. We found that the jets were almost always visible in the 193 and 211 Å channel images. In the "hottest" EUV channels (94 Å, 335 Å), usually the spire of the jet was not visible, although sometimes a base brightening could be discerned. At other wavelengths (171, 131, and 335), the results were mixed. Based on the response characteristics of AIA (Lemen et al, 2011) to the temperature of the observed radiating solar plasma, our finding that most jets are visible in the 193 and 211 Å channels is consistent with other recent studies that measured jet temperatures of 1.5~2.0 MK (Pucci et al, 2012 & Paraschiv et al, 2015). This work was supported by the NASA LWS and HGI programs. Title: Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a CME Authors: Panesar, Navdeep K.; Sterling, Alphonse C.; Innes, Davina E.; Moore, Ronald L. Bibcode: 2015ApJ...811....5P Altcode: 2015arXiv150801952P Homologous flares are flares that occur repetitively in the same active region, with similar structure and morphology. A series of at least eight homologous flares occurred in active region NOAA 11237 over 2011 June 16-17. A nearby prominence/filament was rooted in the active region, and situated near the bottom of a coronal cavity. The active region was on the southeast solar limb as seen from the Solar Dynamics Observatory/Atmospheric Imaging Assembly, and on the disk as viewed from the Solar TErrestrial RElations Observatory/EUVI-B. The dual perspective allows us to study in detail behavior of the prominence/filament material entrained in the magnetic field of the repeatedly erupting system. Each of the eruptions were mainly confined, but expelled hot material into the prominence/filament cavity system (PFCS). The field carrying and containing the ejected hot material interacted with the PFCS and caused it to inflate, resulting in a step-wise rise of the PFCS approximately in step with the homologous eruptions. The eighth eruption triggered the PFCS to move outward slowly, accompanied by a weak coronal dimming. As this slow PFCS eruption was underway, a final “ejective” flare occurred in the core of the active region, resulting in strong dimming in the EUVI-B images and expulsion of a coronal mass ejection (CME). A plausible scenario is that the repeated homologous flares could have gradually destabilized the PFCS, and its subsequent eruption removed field above the acitive region and in turn led to the ejective flare, strong dimming, and CME. Title: Search for Dark Matter in Events with Missing Transverse Momentum and a Higgs Boson Decaying to Two Photons in p p Collisions at √{s }=8 TeV with the ATLAS Detector Authors: Aad, G.; Abbott, B.; Abdallah, J.; Abdinov, O.; Aben, R.; Abolins, M.; Abouzeid, O. S.; Abramowicz, H.; Abreu, H.; Abreu, R.; Abulaiti, Y.; Acharya, B. S.; Adamczyk, L.; Adams, D. L.; Adelman, J.; Adomeit, S.; Adye, T.; Affolder, A. A.; Agatonovic-Jovin, T.; Aguilar-Saavedra, J. A.; Ahlen, S. P.; Ahmadov, F.; Aielli, G.; Akerstedt, H.; Åkesson, T. P. A.; Akimoto, G.; Akimov, A. V.; Alberghi, G. L.; Albert, J.; Albrand, S.; Alconada Verzini, M. J.; Aleksa, M.; Aleksandrov, I. N.; Alexa, C.; Alexander, G.; Alexopoulos, T.; Alhroob, M.; Alimonti, G.; Alio, L.; Alison, J.; Alkire, S. P.; Allbrooke, B. M. M.; Allport, P. P.; Aloisio, A.; Alonso, A.; Alonso, F.; Alpigiani, C.; Altheimer, A.; Alvarez Gonzalez, B.; Álvarez Piqueras, D.; Alviggi, M. G.; Amadio, B. T.; Amako, K.; Amaral Coutinho, Y.; Amelung, C.; Amidei, D.; Amor Dos Santos, S. P.; Amorim, A.; Amoroso, S.; Amram, N.; Amundsen, G.; Anastopoulos, C.; Ancu, L. S.; Andari, N.; Andeen, T.; Anders, C. F.; Anders, G.; Anders, J. K.; Anderson, K. J.; Andreazza, A.; Andrei, V.; Angelidakis, S.; Angelozzi, I.; Anger, P.; Angerami, A.; Anghinolfi, F.; Anisenkov, A. V.; Anjos, N.; Annovi, A.; Antonelli, M.; Antonov, A.; Antos, J.; Anulli, F.; Aoki, M.; Aperio Bella, L.; Arabidze, G.; Arai, Y.; Araque, J. P.; Arce, A. T. H.; Arduh, F. A.; Arguin, J. -F.; Argyropoulos, S.; Arik, M.; Armbruster, A. J.; Arnaez, O.; Arnal, V.; Arnold, H.; Arratia, M.; Arslan, O.; Artamonov, A.; Artoni, G.; Asai, S.; Asbah, N.; Ashkenazi, A.; Åsman, B.; Asquith, L.; Assamagan, K.; Astalos, R.; Atkinson, M.; Atlay, N. B.; Auerbach, B.; Augsten, K.; Aurousseau, M.; Avolio, G.; Axen, B.; Ayoub, M. K.; Azuelos, G.; Baak, M. A.; Baas, A. E.; Bacci, C.; Bachacou, H.; Bachas, K.; Backes, M.; Backhaus, M.; Bagiacchi, P.; Bagnaia, P.; Bai, Y.; Bain, T.; Baines, J. T.; Baker, O. K.; Balek, P.; Balestri, T.; Balli, F.; Banas, E.; Banerjee, Sw.; Bannoura, A. A. E.; Bansil, H. S.; Barak, L.; Barberio, E. L.; Barberis, D.; Barbero, M.; Barillari, T.; Barisonzi, M.; Barklow, T.; Barlow, N.; Barnes, S. L.; Barnett, B. M.; Barnett, R. M.; Barnovska, Z.; Baroncelli, A.; Barone, G.; Barr, A. J.; Barreiro, F.; Barreiro Guimarães da Costa, J.; Bartoldus, R.; Barton, A. E.; Bartos, P.; Basalaev, A.; Bassalat, A.; Basye, A.; Bates, R. L.; Batista, S. J.; Batley, J. R.; Battaglia, M.; Bauce, M.; Bauer, F.; Bawa, H. S.; Beacham, J. B.; Beattie, M. D.; Beau, T.; Beauchemin, P. H.; Beccherle, R.; Bechtle, P.; Beck, H. P.; Becker, K.; Becker, M.; Becker, S.; Beckingham, M.; Becot, C.; Beddall, A. J.; Beddall, A.; Bednyakov, V. A.; Bee, C. P.; Beemster, L. J.; Beermann, T. A.; Begel, M.; Behr, J. K.; Belanger-Champagne, C.; Bell, W. H.; Bella, G.; Bellagamba, L.; Bellerive, A.; Bellomo, M.; Belotskiy, K.; Beltramello, O.; Benary, O.; Benchekroun, D.; Bender, M.; Bendtz, K.; Benekos, N.; Benhammou, Y.; Benhar Noccioli, E.; Benitez Garcia, J. A.; Benjamin, D. P.; Bensinger, J. R.; Bentvelsen, S.; Beresford, L.; Beretta, M.; Berge, D.; Bergeaas Kuutmann, E.; Berger, N.; Berghaus, F.; Beringer, J.; Bernard, C.; Bernard, N. R.; Bernius, C.; Bernlochner, F. U.; Berry, T.; Berta, P.; Bertella, C.; Bertoli, G.; Bertolucci, F.; Bertsche, C.; Bertsche, D.; Besana, M. I.; Besjes, G. J.; Bessidskaia Bylund, O.; Bessner, M.; Besson, N.; Betancourt, C.; Bethke, S.; Bevan, A. J.; Bhimji, W.; Bianchi, R. M.; Bianchini, L.; Bianco, M.; Biebel, O.; Bieniek, S. P.; Biglietti, M.; Bilbao de Mendizabal, J.; Bilokon, H.; Bindi, M.; Binet, S.; Bingul, A.; Bini, C.; Black, C. W.; Black, J. E.; Black, K. M.; Blackburn, D.; Blair, R. E.; Blanchard, J. -B.; Blanco, J. E.; Blazek, T.; Bloch, I.; Blocker, C.; Blum, W.; Blumenschein, U.; Bobbink, G. J.; Bobrovnikov, V. S.; Bocchetta, S. S.; Bocci, A.; Bock, C.; Boehler, M.; Bogaerts, J. A.; Bogdanchikov, A. G.; Bohm, C.; Boisvert, V.; Bold, T.; Boldea, V.; Boldyrev, A. S.; Bomben, M.; Bona, M.; Boonekamp, M.; Borisov, A.; Borissov, G.; Borroni, S.; Bortfeldt, J.; Bortolotto, V.; Bos, K.; Boscherini, D.; Bosman, M.; Boudreau, J.; Bouffard, J.; Bouhova-Thacker, E. V.; Boumediene, D.; Bourdarios, C.; Bousson, N.; Boveia, A.; Boyd, J.; Boyko, I. R.; Bozic, I.; Bracinik, J.; Brandt, A.; Brandt, G.; Brandt, O.; Bratzler, U.; Brau, B.; Brau, J. E.; Braun, H. M.; Brazzale, S. F.; Brendlinger, K.; Brennan, A. J.; Brenner, L.; Brenner, R.; Bressler, S.; Bristow, K.; Bristow, T. M.; Britton, D.; Britzger, D.; Brochu, F. M.; Brock, I.; Brock, R.; Bronner, J.; Brooijmans, G.; Brooks, T.; Brooks, W. K.; Brosamer, J.; Brost, E.; Brown, J.; Bruckman de Renstrom, P. A.; Bruncko, D.; Bruneliere, R.; Bruni, A.; Bruni, G.; Bruschi, M.; Bryngemark, L.; Buanes, T.; Buat, Q.; Buchholz, P.; Buckley, A. G.; Buda, S. I.; Budagov, I. A.; Buehrer, F.; Bugge, L.; Bugge, M. K.; Bulekov, O.; Bullock, D.; Burckhart, H.; Burdin, S.; Burghgrave, B.; Burke, S.; Burmeister, I.; Busato, E.; Büscher, D.; Büscher, V.; Bussey, P.; Butler, J. M.; Butt, A. I.; Buttar, C. M.; Butterworth, J. M.; Butti, P.; Buttinger, W.; Buzatu, A.; Buzykaev, A. R.; Cabrera Urbán, S.; Caforio, D.; Cairo, V. M.; Cakir, O.; Calafiura, P.; Calandri, A.; Calderini, G.; Calfayan, P.; Caloba, L. P.; Calvet, D.; Calvet, S.; Camacho Toro, R.; Camarda, S.; Camarri, P.; Cameron, D.; Caminada, L. M.; Caminal Armadans, R.; Campana, S.; Campanelli, M.; Campoverde, A.; Canale, V.; Canepa, A.; Cano Bret, M.; Cantero, J.; Cantrill, R.; Cao, T.; Capeans Garrido, M. D. M.; Caprini, I.; Caprini, M.; Capua, M.; Caputo, R.; Cardarelli, R.; Carli, T.; Carlino, G.; Carminati, L.; Caron, S.; Carquin, E.; Carrillo-Montoya, G. D.; Carter, J. R.; Carvalho, J.; Casadei, D.; Casado, M. P.; Casolino, M.; Castaneda-Miranda, E.; Castelli, A.; Castillo Gimenez, V.; Castro, N. F.; Catastini, P.; Catinaccio, A.; Catmore, J. R.; Cattai, A.; Caudron, J.; Cavaliere, V.; Cavalli, D.; Cavalli-Sforza, M.; Cavasinni, V.; Ceradini, F.; Cerio, B. C.; Cerny, K.; Cerqueira, A. S.; Cerri, A.; Cerrito, L.; Cerutti, F.; Cerv, M.; Cervelli, A.; Cetin, S. A.; Chafaq, A.; Chakraborty, D.; Chalupkova, I.; Chang, P.; Chapleau, B.; Chapman, J. D.; Charlton, D. G.; Chau, C. C.; Chavez Barajas, C. A.; Cheatham, S.; Chegwidden, A.; Chekanov, S.; Chekulaev, S. V.; Chelkov, G. A.; Chelstowska, M. A.; Chen, C.; Chen, H.; Chen, K.; Chen, L.; Chen, S.; Chen, X.; Chen, Y.; Cheng, H. C.; Cheng, Y.; Cheplakov, A.; Cheremushkina, E.; Cherkaoui El Moursli, R.; Chernyatin, V.; Cheu, E.; Chevalier, L.; Chiarella, V.; Childers, J. T.; Chiodini, G.; Chisholm, A. S.; Chislett, R. T.; Chitan, A.; Chizhov, M. V.; Choi, K.; Chouridou, S.; Chow, B. K. B.; Christodoulou, V.; Chromek-Burckhart, D.; Chu, M. L.; Chudoba, J.; Chuinard, A. J.; Chwastowski, J. J.; Chytka, L.; Ciapetti, G.; Ciftci, A. K.; Cinca, D.; Cindro, V.; Cioara, I. A.; Ciocio, A.; Citron, Z. H.; Ciubancan, M.; Clark, A.; Clark, B. L.; Clark, P. J.; Clarke, R. N.; Cleland, W.; Clement, C.; Coadou, Y.; Cobal, M.; Coccaro, A.; Cochran, J.; Coffey, L.; Cogan, J. G.; Cole, B.; Cole, S.; Colijn, A. P.; Collot, J.; Colombo, T.; Compostella, G.; Conde Muiño, P.; Coniavitis, E.; Connell, S. H.; Connelly, I. A.; Consonni, S. M.; Consorti, V.; Constantinescu, S.; Conta, C.; Conti, G.; Conventi, F.; Cooke, M.; Cooper, B. D.; Cooper-Sarkar, A. M.; Cornelissen, T.; Corradi, M.; Corriveau, F.; Corso-Radu, A.; Cortes-Gonzalez, A.; Cortiana, G.; Costa, G.; Costa, M. J.; Costanzo, D.; Côté, D.; Cottin, G.; Cowan, G.; Cox, B. E.; Cranmer, K.; Cree, G.; Crépé-Renaudin, S.; Crescioli, F.; Cribbs, W. A.; Crispin Ortuzar, M.; Cristinziani, M.; Croft, V.; Crosetti, G.; Cuhadar Donszelmann, T.; Cummings, J.; Curatolo, M.; Cuthbert, C.; Czirr, H.; Czodrowski, P.; D'Auria, S.; D'Onofrio, M.; da Cunha Sargedas de Sousa, M. J.; da Via, C.; Dabrowski, W.; Dafinca, A.; Dai, T.; Dale, O.; Dallaire, F.; Dallapiccola, C.; Dam, M.; Dandoy, J. R.; Dang, N. P.; Daniells, A. C.; Danninger, M.; Dano Hoffmann, M.; Dao, V.; Darbo, G.; Darmora, S.; Dassoulas, J.; Dattagupta, A.; Davey, W.; David, C.; Davidek, T.; Davies, E.; Davies, M.; Davison, P.; Davygora, Y.; Dawe, E.; Dawson, I.; Daya-Ishmukhametova, R. K.; de, K.; de Asmundis, R.; de Castro, S.; de Cecco, S.; de Groot, N.; de Jong, P.; de la Torre, H.; de Lorenzi, F.; de Nooij, L.; de Pedis, D.; de Salvo, A.; de Sanctis, U.; de Santo, A.; de Vivie de Regie, J. B.; Dearnaley, W. J.; Debbe, R.; Debenedetti, C.; Dedovich, D. V.; Deigaard, I.; Del Peso, J.; Del Prete, T.; Delgove, D.; Deliot, F.; Delitzsch, C. M.; Deliyergiyev, M.; Dell'Acqua, A.; Dell'Asta, L.; Dell'Orso, M.; Della Pietra, M.; Della Volpe, D.; Delmastro, M.; Delsart, P. A.; Deluca, C.; Demarco, D. A.; Demers, S.; Demichev, M.; Demilly, A.; Denisov, S. P.; Derendarz, D.; Derkaoui, J. E.; Derue, F.; Dervan, P.; Desch, K.; Deterre, C.; Deviveiros, P. O.; Dewhurst, A.; Dhaliwal, S.; di Ciaccio, A.; di Ciaccio, L.; di Domenico, A.; di Donato, C.; di Girolamo, A.; di Girolamo, B.; di Mattia, A.; di Micco, B.; di Nardo, R.; di Simone, A.; di Sipio, R.; di Valentino, D.; Diaconu, C.; Diamond, M.; Dias, F. A.; Diaz, M. A.; Diehl, E. B.; Dietrich, J.; Diglio, S.; Dimitrievska, A.; Dingfelder, J.; Dita, P.; Dita, S.; Dittus, F.; Djama, F.; Djobava, T.; Djuvsland, J. I.; Do Vale, M. A. B.; Dobos, D.; Dobre, M.; Doglioni, C.; Dohmae, T.; Dolejsi, J.; Dolezal, Z.; Dolgoshein, B. A.; Donadelli, M.; Donati, S.; Dondero, P.; Donini, J.; Dopke, J.; Doria, A.; Dova, M. T.; Doyle, A. T.; Drechsler, E.; Dris, M.; Dubreuil, E.; Duchovni, E.; Duckeck, G.; Ducu, O. A.; Duda, D.; Dudarev, A.; Duflot, L.; Duguid, L.; Dührssen, M.; Dunford, M.; Duran Yildiz, H.; Düren, M.; Durglishvili, A.; Duschinger, D.; Dyndal, M.; Eckardt, C.; Ecker, K. M.; Edgar, R. C.; Edson, W.; Edwards, N. C.; Ehrenfeld, W.; Eifert, T.; Eigen, G.; Einsweiler, K.; Ekelof, T.; El Kacimi, M.; Ellert, M.; Elles, S.; Ellinghaus, F.; Elliot, A. A.; Ellis, N.; Elmsheuser, J.; Elsing, M.; Emeliyanov, D.; Enari, Y.; Endner, O. C.; Endo, M.; Erdmann, J.; Ereditato, A.; Ernis, G.; Ernst, J.; Ernst, M.; Errede, S.; Ertel, E.; Escalier, M.; Esch, H.; Escobar, C.; Esposito, B.; Etienvre, A. I.; Etzion, E.; Evans, H.; Ezhilov, A.; Fabbri, L.; Facini, G.; Fakhrutdinov, R. M.; Falciano, S.; Falla, R. J.; Faltova, J.; Fang, Y.; Fanti, M.; Farbin, A.; Farilla, A.; Farooque, T.; Farrell, S.; Farrington, S. M.; Farthouat, P.; Fassi, F.; Fassnacht, P.; Fassouliotis, D.; Faucci Giannelli, M.; Favareto, A.; Fayard, L.; Federic, P.; Fedin, O. L.; Fedorko, W.; Feigl, S.; Feligioni, L.; Feng, C.; Feng, E. J.; Feng, H.; Fenyuk, A. B.; Fernandez Martinez, P.; Fernandez Perez, S.; Ferrando, J.; Ferrari, A.; Ferrari, P.; Ferrari, R.; Ferreira de Lima, D. E.; Ferrer, A.; Ferrere, D.; Ferretti, C.; Ferretto Parodi, A.; Fiascaris, M.; Fiedler, F.; Filipčič, A.; Filipuzzi, M.; Filthaut, F.; Fincke-Keeler, M.; Finelli, K. D.; Fiolhais, M. C. N.; Fiorini, L.; Firan, A.; Fischer, A.; Fischer, C.; Fischer, J.; Fisher, W. C.; Fitzgerald, E. A.; Flechl, M.; Fleck, I.; Fleischmann, P.; Fleischmann, S.; Fletcher, G. T.; Fletcher, G.; Flick, T.; Floderus, A.; Flores Castillo, L. R.; Flowerdew, M. J.; Formica, A.; Forti, A.; Fournier, D.; Fox, H.; Fracchia, S.; Francavilla, P.; Franchini, M.; Francis, D.; Franconi, L.; Franklin, M.; Fraternali, M.; Freeborn, D.; French, S. T.; Friedrich, F.; Froidevaux, D.; Frost, J. A.; Fukunaga, C.; Fullana Torregrosa, E.; Fulsom, B. G.; Fuster, J.; Gabaldon, C.; Gabizon, O.; Gabrielli, A.; Gabrielli, A.; Gadatsch, S.; Gadomski, S.; Gagliardi, G.; Gagnon, P.; Galea, C.; Galhardo, B.; Gallas, E. J.; Gallop, B. J.; Gallus, P.; Galster, G.; Gan, K. K.; Gao, J.; Gao, Y.; Gao, Y. S.; Garay Walls, F. M.; Garberson, F.; García, C.; García Navarro, J. E.; Garcia-Sciveres, M.; Gardner, R. W.; Garelli, N.; Garonne, V.; Gatti, C.; Gaudiello, A.; Gaudio, G.; Gaur, B.; Gauthier, L.; Gauzzi, P.; Gavrilenko, I. L.; Gay, C.; Gaycken, G.; Gazis, E. N.; Ge, P.; Gecse, Z.; Gee, C. N. P.; Geerts, D. A. A.; Geich-Gimbel, Ch.; Geisler, M. P.; Gemme, C.; Genest, M. H.; Gentile, S.; George, M.; George, S.; Gerbaudo, D.; Gershon, A.; Ghazlane, H.; Giacobbe, B.; Giagu, S.; Giangiobbe, V.; Giannetti, P.; Gibbard, B.; Gibson, S. M.; Gilchriese, M.; Gillam, T. P. S.; Gillberg, D.; Gilles, G.; Gingrich, D. M.; Giokaris, N.; Giordani, M. P.; Giorgi, F. M.; Giorgi, F. M.; Giraud, P. F.; Giromini, P.; Giugni, D.; Giuliani, C.; Giulini, M.; Gjelsten, B. K.; Gkaitatzis, S.; Gkialas, I.; Gkougkousis, E. L.; Gladilin, L. K.; Glasman, C.; Glatzer, J.; Glaysher, P. C. F.; Glazov, A.; Goblirsch-Kolb, M.; Goddard, J. 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M.; Zalieckas, J.; Zaman, A.; Zambito, S.; Zanello, L.; Zanzi, D.; Zeitnitz, C.; Zeman, M.; Zemla, A.; Zengel, K.; Zenin, O.; Ženiš, T.; Zerwas, D.; Zhang, D.; Zhang, F.; Zhang, J.; Zhang, L.; Zhang, R.; Zhang, X.; Zhang, Z.; Zhao, X.; Zhao, Y.; Zhao, Z.; Zhemchugov, A.; Zhong, J.; Zhou, B.; Zhou, C.; Zhou, L.; Zhou, L.; Zhou, N.; Zhu, C. G.; Zhu, H.; Zhu, J.; Zhu, Y.; Zhuang, X.; Zhukov, K.; Zibell, A.; Zieminska, D.; Zimine, N. I.; Zimmermann, C.; Zimmermann, S.; Zinonos, Z.; Zinser, M.; Ziolkowski, M.; Živković, L.; Zobernig, G.; Zoccoli, A.; Zur Nedden, M.; Zurzolo, G.; Zwalinski, L.; Atlas Collaboration Bibcode: 2015PhRvL.115m1801A Altcode: 2015arXiv150601081A Results of a search for new phenomena in events with large missing transverse momentum and a Higgs boson decaying to two photons are reported. Data from proton-proton collisions at a center-of-mass energy of 8 TeV and corresponding to an integrated luminosity of 20.3 fb-1 have been collected with the ATLAS detector at the LHC. The observed data are well described by the expected standard model backgrounds. Upper limits on the cross section of events with large missing transverse momentum and a Higgs boson candidate are also placed. Exclusion limits are presented for models of physics beyond the standard model featuring dark-matter candidates. Title: Small-scale filament eruptions as the driver of X-ray jets in solar coronal holes Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Adams, Mitzi Bibcode: 2015Natur.523..437S Altcode: 2017arXiv170503373S Solar X-ray jets are thought to be made by a burst of reconnection of closed magnetic field at the base of a jet with ambient open field. In the accepted version of the `emerging-flux' model, such a reconnection occurs at a plasma current sheet between the open field and the emerging closed field, and also forms a localized X-ray brightening that is usually observed at the edge of the jet's base. Here we report high-resolution X-ray and extreme-ultraviolet observations of 20 randomly selected X-ray jets that form in coronal holes at the Sun's poles. In each jet, contrary to the emerging-flux model, a miniature version of the filament eruptions that initiate coronal mass ejections drives the jet-producing reconnection. The X-ray bright point occurs by reconnection of the `legs' of the minifilament-carrying erupting closed field, analogous to the formation of solar flares in larger-scale eruptions. Previous observations have found that some jets are driven by base-field eruptions, but only one such study, of only one jet, provisionally questioned the emerging-flux model. Our observations support the view that solar filament eruptions are formed by a fundamental explosive magnetic process that occurs on a vast range of scales, from the biggest mass ejections and flare eruptions down to X-ray jets, and perhaps even down to smaller jets that may power coronal heating. A similar scenario has previously been suggested, but was inferred from different observations and based on a different origin of the erupting minifilament. Title: Near-Sun speed of CMEs and the magnetic nonpotentiality of their source active regions Authors: Tiwari, Sanjiv K.; Falconer, David A.; Moore, Ronald L.; Venkatakrishnan, P.; Winebarger, Amy R.; Khazanov, Igor G. Bibcode: 2015GeoRL..42.5702T Altcode: 2015arXiv150801532T We show that the speed of the fastest coronal mass ejections (CMEs) that an active region (AR) can produce can be predicted from a vector magnetogram of the AR. This is shown by logarithmic plots of CME speed (from the SOHO Large Angle and Spectrometric Coronagraph CME catalog) versus each of ten AR-integrated magnetic parameters (AR magnetic flux, three different AR magnetic-twist parameters, and six AR free-magnetic-energy proxies) measured from the vertical and horizontal field components of vector magnetograms (from the Solar Dynamics Observatory's Helioseismic and Magnetic Imager) of the source ARs of 189 CMEs. These plots show the following: (1) the speed of the fastest CMEs that an AR can produce increases with each of these whole-AR magnetic parameters and (2) that one of the AR magnetic-twist parameters and the corresponding free-magnetic-energy proxy each determine the CME-speed upper limit line somewhat better than any of the other eight whole-AR magnetic parameters. Title: Magnetic Untwisting in Solar Jets that Go into the Outer Corona in Polar Coronal Holes Authors: Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David A. Bibcode: 2015ApJ...806...11M Altcode: 2015arXiv150403700M We study 14 large solar jets observed in polar coronal holes. In EUV movies from the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), each jet appears similar to most X-ray jets and EUV jets that erupt in coronal holes; but each is exceptional in that it goes higher than most, so high that it is observed in the outer corona beyond 2.2 R Sun in images from the Solar and Heliospheric Observatory/Large Angle Spectroscopic Coronagraph (LASCO)/C2 coronagraph. From AIA He ii 304 Å movies and LASCO/C2 running-difference images of these high-reaching jets, we find: (1) the front of the jet transits the corona below 2.2 R Sun at a speed typically several times the sound speed; (2) each jet displays an exceptionally large amount of spin as it erupts; (3) in the outer corona, most of the jets display measureable swaying and bending of a few degrees in amplitude; in three jets the swaying is discernibly oscillatory with a period of order 1 hr. These characteristics suggest that the driver in these jets is a magnetic-untwisting wave that is basically a large-amplitude (i.e., nonlinear) torsional Alfvén wave that is put into the reconnected open field in the jet by interchange reconnection as the jet erupts. From the measured spinning and swaying, we estimate that the magnetic-untwisting wave loses most of its energy in the inner corona below 2.2 R Sun. We point out that the torsional waves observed in Type-II spicules might dissipate in the corona in the same way as the magnetic-untwisting waves in our big jets, and thereby power much of the coronal heating in coronal holes. Title: Small-Scale Filament Eruptions Leading to Solar X-Ray Jets Authors: Sterling, Alphonse; Moore, Ronald; Falconer, David Bibcode: 2015TESS....140701S Altcode: We investigate the onset of ~10 random X-ray jets observed by Hinode/XRT. Each jet was near the limb in a polar coronal hole, and showed a ``bright point'' in an edge of the base of the jet, as is typical for previously-observed X-ray jets. We examined SDO/AIA EUV images of each of the jets over multiple AIA channels, including 304 Å, which detects chromospheric emissions, and 171, 193, and 211 Å, which detect cooler-coronal emissions. We find the jets to result from eruptions of miniature (size <~10 arcsec) filaments from the bases of the jets. Much of the erupting-filament material forms a chromospheric-temperature jet. In the cool-coronal channels, often the filament appears in absorption and the hotter EUV component of the jet appears in emission. The jet bright point forms at the location from which the miniature filament erupts, analogous to the formation of a standard solar flare arcade in the wake of the eruption of a typical larger-scalechromospheric filament. The spire of the jet forms on open field lines that presumably have undergone interchange reconnection with the erupting field that envelops and carries the miniature filament. Thus these X-ray jets and their bright points are made by miniature filament eruptions via ``internal'' and ``external'' reconnection of the erupting field. This is consistent with what we found for the onset of an on-disk coronal jet we examined in Adams et al. (2014). This work was supported by funding from NASA/LWS, Hinode, and ISSI. Title: A Prominence/filament eruption triggered by eight homologous flares Authors: Panesar, Navdeep K.; Sterling, Alphonse; Innes, Davina; Moore, Ronald Bibcode: 2015TESS....140805P Altcode: Eight homologous flares occurred in active region NOAA 11237 over 16 - 17 June 2011. A prominence system with a surrounding coronal cavity was adjacent to, but still magnetically connected to the active region. The eight eruptions expelled hot material from the active region into the prominence/filament cavity system (PFCS) where the ejecta became confined. We mainly aim to diagnose the 3D dynamics of the PFCS during the series of eight homologous eruptions by using data from two instruments: SDO/AIA and STEREO/EUVI-B, covering the Sun from two directions. The field containing the ejected hot material interacts with the PFCS and causes it to inflate, resulting in a discontinuous rise of the prominence/filament approximately in steps with the homologous eruptions. The eighth eruption triggers the PFCS to move outward slowly, accompanied by a weak coronal dimming. Subsequently the prominence/filament material drains to the solar surface. This PFCS eruption evidently slowly opens field overlying the active region, which results in a final ‘ejective’ eruption from the core of the active region. A strong dimming appears adjacent to the final eruption’s flare loops in the EUVI-B images, followed by a CME. We propose that the eight homologous flares gradually disrupted the PFCS and removed the overlying field above the active region, leading to the CME via the ‘lid removal’ mechanism. Title: More Macrospicule Jets in On-Disk Coronal Holes Authors: Adams, Mitzi; Sterling, Alphonse; Moore, Ronald Bibcode: 2015TESS....120301A Altcode: We examine the magnetic structure and dynamics of multiple jets found in coronal holes close to or at disk center. All data are from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory (SDO). We report on observations of about ten jets in an equatorial coronal hole spanning 2011 February 27 and 28. We show the evolution of these jets in AIA 193 Å, examine the magnetic field configuration and flux changes in the jet area, and discuss the probable trigger mechanism of these events. We reported on another jet in this same coronal hole on 2011 February 27, ~13:04 UT (Adams et al 2014, ApJ, 783: 11). That jet is a previously unrecognized variety of blowout jet, in which the base-edge bright point is a miniature filament-eruption flare arcade made by internal reconnection of the legs of the erupting field. In contrast, in the presently-accepted "standard" picture for blowout jets, the base-edge bright point is made by interchange reconnection of initially-closed erupting jet-base field with ambient open field. This poster presents further evidence of the production of the base-edge bright point in blowout jets by internal reconnection. Our observations suggest that most of the bigger and brighter EUV jets in coronal holes are blowout jets of the new-found variety. Title: Evidence of suppressed heating of coronal loops rooted in opposite polarity sunspot umbrae Authors: Tiwari, Sanjiv K.; Thalmann, Julia K.; Winebarger, Amy R.; Panesar, Navdeep K.; Moore, Ronald Bibcode: 2015TESS....120404T Altcode: Observations of active region (AR) coronae in different EUV wavelengths reveal the presence of various loops at different temperatures. To understand the mechanisms that result in hotter or cooler loops, we study a typical bipolar AR, near solar disk center, which has moderate overall magnetic twist and at least one fully developed sunspot of each polarity. From AIA 193 and 94 A images we identify many clearly discernible coronal loops that connect opposite-polarity plage or a sunspot to a opposite-polarity plage region. The AIA 94 A images show dim regions in the umbrae of the spots. To see which coronal loops are rooted in a dim umbral area, we performed a non-linear force-free field (NLFFF) modeling using photospheric vector magnetic field measurements obtained with the Heliosesmic Magnetic Imager (HMI) onboard SDO. After validation of the NLFFF model by comparison of calculated model field lines and observed loops in AIA 193 and 94 A, we specify the photospheric roots of the model field lines. The model field then shows the coronal magnetic loops that arch from the dim umbral area of the positive-polarity sunspot to the dim umbral area of a negative-polarity sunspot. Because these coronal loops are not visible in any of the coronal EUV and X-ray images of the AR, we conclude they are the coolest loops in the AR. This result suggests that the loops connecting opposite polarity umbrae are the least heated because the field in umbrae is so strong that the convective braiding of the field is strongly suppressed.From this result, we further hypothesize that the convective freedom at the feet of a coronal loop, together with the strength of the field in the body of the loop, determines the strength of the heating. In particular, we expect the hottest coronal loops to have one foot in an umbra and the other foot in opposite-polarity penumbra or plage (coronal moss), the areas of strong field in which convection is not as strongly suppressed as in umbrae. Many transient, outstandingly bright, loops in the AIA 94 A movie of the AR do have this expected rooting pattern. Title: Center-to-Limb Variation of Deprojection Errors in SDO/HMI Vector Magnetograms Authors: Falconer, David; Moore, Ronald; Barghouty, Nasser; Tiwari, Sanjiv K.; Khazanov, Igor Bibcode: 2015TESS....140204F Altcode: For use in investigating the magnetic causes of coronal heating in active regions and for use in forecasting an active region’s productivity of major CME/flare eruptions, we have evaluated various sunspot-active-region magnetic measures (e.g., total magnetic flux, free-magnetic-energy proxies, magnetic twist measures) from HMI Active Region Patches (HARPs) after the HARP has been deprojected to disk center. From a few tens of thousand HARP vector magnetograms (of a few hundred sunspot active regions) that have been deprojected to disk center, we have determined that the errors in the whole-HARP magnetic measures from deprojection are negligibly small for HARPS deprojected from distances out to 45 heliocentric degrees. For some purposes the errors from deprojection are tolerable out to 60 degrees. We obtained this result by the following process. For each whole-HARP magnetic measure: 1) for each HARP disk passage, normalize the measured values by the measured value for that HARP at central meridian; 2) then for each 0.05 Rs annulus, average the values from all the HARPs in the annulus. This results in an average normalized value as a function of radius for each measure. Assuming no deprojection errors and that, among a large set of HARPs, the measure is as likely to decrease as to increase with HARP distance from disk center, the average of each annulus is expected to be unity, and, for a statistically large sample, the amount of deviation of the average from unity estimates the error from deprojection effects. The deprojection errors arise from 1) errors in the transverse field being deprojected into the vertical field for HARPs observed at large distances from disk center, 2) increasingly larger foreshortening at larger distances from disk center, and 3) possible errors in transverse-field-direction ambiguity resolution.From the compiled set of measured vales of whole-HARP magnetic nonpotentiality parameters measured from deprojected HARPs, we have examined the relation between each nonpotentiality parameter and the speed of CMEs from the measured active regions. For several different nonpotentiality parameters we find there is an upper limit to the CME speed, the limit increasing as the value of the parameter increases. Title: Reconnection and Spire Drift in Coronal Jets Authors: Moore, Ronald; Sterling, Alphonse; Falconer, David Bibcode: 2015TESS....140702M Altcode: It is observed that there are two morphologically-different kinds of X-ray/EUV jets in coronal holes: standard jets and blowout jets. In both kinds: (1) in the base of the jet there is closed magnetic field that has one foot in flux of polarity opposite that of the ambient open field of the coronal hole, and (2) in coronal X-ray/EUV images of the jet there is typically a bright nodule at the edge of the base. In the conventional scenario for jets of either kind, the bright nodule is a compact flare arcade, the downward product of interchange reconnection of closed field in the base with impacted ambient open field, and the upper product of this reconnection is the jet-outflow spire. It is also observed that in most jets of either kind the spire drifts sideways away from the bright nodule. We present the observed bright nodule and spire drift in an example standard jet and in two example blowout jets. With cartoons of the magnetic field and its reconnection in jets, we point out: (1) if the bright nodule is a compact flare arcade made by interchange reconnection, then the spire should drift toward the bright nodule, and (2) if the bright nodule is instead a compact flare arcade made, as in a filament-eruption flare, by internal reconnection of the legs of the erupting sheared-field core of a lobe of the closed field in the base, then the spire, made by the interchange reconnection that is driven on the outside of that lobe by the lobe’s internal convulsion, should drift away from the bright nodule. Therefore, from the observation that the spire usually drifts away from the bright nodule, we infer: (1) in X-ray/EUV jets of either kind in coronal holes the interchange reconnection that generates the jet-outflow spire usually does not make the bright nodule; instead, the bright nodule is made by reconnection inside erupting closed field in the base, as in a filament eruption, the eruption being either a confined eruption for a standard jet or a blowout eruption (as in a CME) for a blowout jet, and (2) in this respect, the conventional reconnection picture for the bright nodule in coronal jets is usually wrong for observed coronal jets of either kind. Title: Exploring Euv Spicules Using 304 Ang He II Data from SDO/AIA Authors: Snyder, I. R.; Sterling, A. C.; Falconer, D. A.; Moore, R. L. Bibcode: 2014AGUFMSH51C4179S Altcode: We present results from an exploratory study of He II 304 ŠEUV spicules at the limb of the Sun. We also measured properties of one macrospicule; macrospicules are longer than most spicules, and much broader in width than spicules. We use high-cadence (12 sec) and high-resolution (0.6 arcsec pixels) data from the Atmospheric Imaging Array (AIA) instrument on the Solar Dynamic Observatory (SDO). All of the observed events occurred near the solar north pole, in quiet-Sun or coronal-hole environments. We examined the maximum lengths, maximum rise velocities, and lifetimes of about 30 EUV spicules and the macrospicule. For the bulk of the EUV spicules the ranges of these quantities are respectively ~10,000----40,000 km, 20---100 km/s, and ~100--- ~600 sec. For the macrospicule the corresponding quantities are respectively ~60,000 km, ~130 km/s, and ~1800 sec, which is typical of macrospicules measured by other workers. Therefore macrospicules are taller, longer-lived, and faster than most EUV spicules. The rise profiles of both the spicules and the macrospicules fit well to a second-order ("parabolic'') trajectory, although the acceleration was often weaker than that of solar gravity in the profiles fitted to the trajectories. Our macrospicule also had an obvious brightening at its base at birth, whereas such brightenings were not apparent for the EUV spicules. Most of the EUV spicules remained visible during their decent back to the solar surface, although a small percentage of the spicules and the macrospicule faded out before falling back to the surface. Our sample of macrospicules is not yet large enough to address whether they are scaled-up versions of EUV spicules, or independent phenomena. A.C.S. and R.L.M. were supported by funding from the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program, and the Hinode Project. I.R.S. was supported by NSF's Research Experience for Undergraduates Program. Title: Speed of CMEs and the magnetic non-potentiality of their source active regions Authors: Tiwari, S. K.; Falconer, D. A.; Moore, R. L.; Venkatakrishnan, P. Bibcode: 2014AGUFMSH21C4134T Altcode: Most fast coronal mass ejections (CMEs) originate from solar active regions (ARs). Non-potentiality of ARs is expected to determine the speed and size of CMEs in the outer corona. Several other unexplored parameters might be important as well. To find out the correlation between the initial speed of CMEs and the non-potentiality of source ARs, we associated over a hundred of CMEs with source ARs via their co-produced flares. The speed of the CMEs are collected from the SOHO LASCO CME catalog. We have used vector magnetograms obtained mainly with HMI/SDO, also with Hinode (SOT/SP) when available within an hour of a CME occurence, to evaluate various magnetic non-potentiality parameters, e.g. magnetic free-energy proxies, computed magnetic free energy, twist, shear angle, signed shear angle etc. We have also included several other parameters e.g. total unsigned flux, net current, magnetic area of ARs, area of sunspots, to investigate their correlation, if any, with the initial speeds of CMEs. Our preliminary results show that the ARs with larger non-potentiality and area mostly produce fast CMEs but they can also produce slower ones. The ARs with lesser non-potentiality and area generally produce only slower CMEs, however, there are a few exceptions. The total unsigned flux correlate with the non-potentiality parameters and area of ARs but some ARs with large unsigned flux are also found to be least non-potential. A more detailed analysis is underway. SKT is supported by an appointment to the NASA Postdoctoral Program at the NASA Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. RLM is supported by funding from the Living With a Star Targeted Research and Technology Program of the Heliophysics Division of NASA's Science Mission Directorate. Support for MAG4 development comes from NASA's Game Changing Development Program, and Johnson Space Center's Space Radiation Analysis Group (SRAG). Title: Macrospicule Jets in On-Disk Coronal Holes Authors: Adams, M.; Sterling, A. C.; Moore, R. L. Bibcode: 2014AGUFMSH51C4178A Altcode: We examine the magnetic structure and dynamics of multiple jets found in coronal holes close to or on disk center. All data are from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory (SDO). We report on observations of ten jets in an equatorial coronal hole from 2011 February 27 and multiple jets found in equatorial coronal holes on these dates: 2010-June-4, 2012-March-13, 2013-May 29-2013, and 2014-February-24. We will show in detail the evolution of the jets and will compare the magnetic field arrangement and probable trigger mechanism of these events to those of a specific macrospicule jet observed on 2011 February 27. We recently discovered that this jet is a previously-unrecognized variety of blowout jet (Adams et al 2014, ApJ, 783: 11). In this variety, the reconnection bright point is not made by interchange reconnection of initially-closed erupting field in the base of the jet with ambient open field but is a miniature filament-eruption flare arcade made by internal reconnection of the legs of the erupting field. Title: Exploring He II 304 Å Spicules and Macrospicules at the Solar Limb Authors: Sterling, A. C.; Snyder, I. R.; Falconer, D. A.; Moore, R. L. Bibcode: 2014AGUFMSH53D..04S Altcode: We present results from a study of He II 304 Ang spicules and macrospiculesobserved at the limb of the Sun in 304 Ang channel image sequences from theAtmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO). Thesedata have both high spatial (0.6 arcsec pixels) and temporal (12 s) resolution. All of the observed events occurred in quiet or coronal hole regions near the solarpole. He II 304 Ang spicules and macrospicules are both transient jet-likefeatures, with the macrospicules being wider and having taller maximum heights thanthe spicules. We looked for characteristics of the populations of these twophenomena that might indicate whether they have the same initiation mechanisms. Weexamine the maximum heights, time-averaged rise velocities, and lifetimes of about30 spicules and about five macrospicules. For the spicules, these quantities are,respectively, ~10,000----40,000 km, 20---100 km/s, and a few 100--- ~600 sec. Forthe macrospicules the corresponding properties are >~60,000 km, >~55 km/s, andlifetimes of >~1800 sec. Therefore the macrospicules have velocities comparable tothose of the fastest spicules and live longer than the spicules. The leading-edgetrajectories of both the spicules and the macrospicules match well a second-order(``parabolic'') profile, although the acceleration in the fitted profiles is generally weaker than that of solar gravity. The macrospicules also have obviousbrightenings at their bases at their birth, while such brightenings are notapparent for most of the spicules. Our findings are suggestive of the twophenomena possibly having different initiation mechanisms, but this is not yetconclusive. A.C.S. and R.L.M. were supported by funding from the HeliophysicsDivision of NASA's Science Mission Directorate through the Living With a StarTargeted Research and Technology Program, and the Hinode Project. I.R.S. wassupported by NSF's Research Experience for Undergraduates Program. Title: Hi-C Observations of Penumbral Bright Dots Authors: Alpert, S.; Tiwari, S. K.; Moore, R. L.; Savage, S. L.; Winebarger, A. R. Bibcode: 2014AGUFMSH51C4182A Altcode: We use high-quality data obtained by the High Resolution Coronal Imager (Hi-C) to examine bright dots (BDs) in a sunspot's penumbra. The sizes of these BDs are on the order of 1 arcsecond (1") and are therefore hard to identify using the Atmospheric Imaging Assembly's (AIA) 0.6" pixel-1 resolution. These BDs become readily apparent with Hi-C's 0.1" pixel-1 resolution. Tian et al. (2014) found penumbral BDs in the transition region (TR) by using the Interface Region Imaging Spectrograph (IRIS). However, only a few of their dots could be associated with any enhanced brightness in AIA channels. In this work, we examine the characteristics of the penumbral BDs observed by Hi-C in a sunspot penumbra, including their sizes, lifetimes, speeds, and intensity. We also attempt to relate these BDs to the IRIS BDs. There are fewer Hi-C BDs in the penumbra than seen by IRIS, though different sunspots were studied. We use 193Å Hi-C data from July 11, 2012 which observed from ~18:52:00 UT--18:56:00 UT and supplement it with data from AIA's 193Å passband to see the complete lifetime of the dots that were born before and/or lasted longer than Hi-C's 5-minute observation period. We use additional AIA passbands and compare the light curves of the BDs at different temperatures to test whether the Hi-C BDs are TR BDs. We find that most Hi-C BDs show clear movement, and of those that do, they move in a radial direction, toward or away from the sunspot umbra. Single BDs interact with other BDs, combining to fade away or brighten. The BDs that do not interact with other BDs tend to move less. Our BDs are similar to the exceptional IRIS BDs: they move slower on average and their sizes and lifetimes are on the high end of the distribution of IRIS BDs. We infer that our penumbral BDs are some of the larger BDs observed by IRIS, those that are bright enough in TR emission to be seen in the 193Å band of Hi-C. Title: Trigger Mechanism of Solar Subflares in a Braided Coronal Magnetic Structure Authors: Tiwari, Sanjiv K.; Alexander, Caroline E.; Winebarger, Amy R.; Moore, Ronald L. Bibcode: 2014ApJ...795L..24T Altcode: 2014arXiv1410.4260T Fine-scale braiding of coronal magnetic loops by continuous footpoint motions may power coronal heating via nanoflares, which are spontaneous fine-scale bursts of internal reconnection. An initial nanoflare may trigger an avalanche of reconnection of the braids, making a microflare or larger subflare. In contrast to this internal triggering of subflares, we observe external triggering of subflares in a braided coronal magnetic field observed by the High-resolution Coronal Imager (Hi-C). We track the development of these subflares using 12 s cadence images acquired by SDO/AIA in 1600, 193, 94 Å, and registered magnetograms of SDO/HMI, over four hours centered on the Hi-C observing time. These data show numerous recurring small-scale brightenings in transition-region emission happening on polarity inversion lines where flux cancellation is occurring. We present in detail an example of an apparent burst of reconnection of two loops in the transition region under the braided coronal field which is appropriate for releasing a short reconnected loop downward and a longer reconnected loop upward. The short loop presumably submerges into the photosphere, participating in observed flux cancellation. A subflare in the overlying braided magnetic field is apparently triggered by the disturbance of the braided field by the reconnection-released upward loop. At least 10 subflares observed in this braided structure appear to be triggered this way. How common this external trigger mechanism for coronal subflares is in other active regions, and how important it is for coronal heating in general, remain to be seen. Title: New Aspects of a Lid-removal Mechanism in the Onset of an Eruption Sequence that Produced a Large Solar Energetic Particle (SEP) Event Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Knox, Javon M. Bibcode: 2014ApJ...788L..20S Altcode: We examine a sequence of two ejective eruptions from a single active region on 2012 January 23, using magnetograms and EUV images from the Solar Dynamics Observatory's (SDO) Helioseismic and Magnetic Imager (HMI) and Atmospheric and Imaging Assembly (AIA), and EUV images from STEREO/EUVI. This sequence produced two coronal mass ejections (CMEs) and a strong solar energetic particle event (SEP); here we focus on the magnetic onset of this important space weather episode. Cheng et al. showed that the first eruption's ("Eruption 1") flux rope was apparent only in "hotter" AIA channels, and that it removed overlying field that allowed the second eruption ("Eruption 2") to begin via ideal MHD instability; here we say that Eruption 2 began via a "lid removal" mechanism. We show that during Eruption 1's onset, its flux rope underwent a "tether weakening" (TW) reconnection with field that arched from the eruption-source active region to an adjacent active region. Standard flare loops from Eruption 1 developed over Eruption 2's flux rope and enclosed filament, but these overarching new loops were unable to confine that flux rope/filament. Eruption 1's flare loops, from both TW reconnection and standard-flare-model internal reconnection, were much cooler than Eruption 2's flare loops (GOES thermal temperatures of ~7.5 MK and 9 MK, compared to ~14 MK). The corresponding three sequential GOES flares were, respectively, due to TW reconnection plus earlier phase Eruption 1 tether-cutting reconnection, Eruption 1 later-phase tether-cutting reconnection, and Eruption 2 tether-cutting reconnection. Title: MAG4 versus Alternative Techniques for Forecasting Active-Region Flare Productivity Authors: Falconer, David; Moore, Ronald L.; Barghouty, Abdulnasser F; Khazanov, Igor Bibcode: 2014AAS...22440204F Altcode: MAG4 is a technique of forecasting an active region's rate of production of major flares in the coming few days from a free-magnetic-energy proxy. We present a statistical method of measuring the difference in performance between MAG4 and comparable alternative techniques that forecast an active region’s major-flare productivity from alternative observed aspects of the active region. We demonstrate the method by measuring the difference in performance between the “Present MAG4” technique and each of three alternative techniques, called “McIntosh Active-Region Class,” “Total Magnetic Flux,” and “Next MAG4.” We do this by using (1) the MAG4 database of magnetograms and major-flare histories of sunspot active regions, (2) the NOAA table of the major-flare productivity of each of 60 McIntosh active-region classes of sunspot active regions, and (3) five technique-performance metrics (Heidke Skill Score, True Skill Score, Percent Correct, Probability of Detection, and False Alarm Rate) evaluated from 2000 random two-by-two contingency tables obtained from the databases. We find that (1) Present MAG4 far outperforms both McIntosh Active-Region Class and Total Magnetic Flux, (2) Next MAG4 significantly outperforms Present MAG4, (3) the performance of Next MAG4 is insensitive to the forward and backward temporal windows used, in the range of one to a few days, and (4) forecasting from the free-energy proxy in combination with either any broad category of McIntosh active-region classes or any Mount Wilson active-region class gives no significant performance improvement over forecasting from the free-energy proxy alone (Present MAG4). Funding for this research came from NASA’s Game Changing Development Program, Johnson Space Center’s Space Radiation Analysis Group (SRAG), and AFOSR’s Multi-University Research Initiative. In particular, funding was facilitated by Dr. Dan Fry (NASA-JSC) and David Moore (NASA-LaRC). Title: New Aspects of a Lid-Removal Mechanism in the Onset of a SEP-Producing Eruption Sequence Authors: Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David; Knox, Javon M Bibcode: 2014AAS...22421202S Altcode: We examine a sequence of two ejective eruptions from a single active region on 2012 January 23, using magnetograms and EUV images from SDO/HMI and SDO/AIA, and EUV images from STEREO. Cheng et al. (2013) showed that the first eruption's (``Eruption 1'') flux rope was apparent only in ``hotter'' AIA channels, and that it removed overlying field that allowed the second eruption (``Eruption 2'') to begin via ideal MHD instability; here we say Eruption 2 began via a ``lid removal'' mechanism. We show that during Eruption-1's onset, its flux rope underwent ``tether weakening'' (TW) reconnection with the field of an adjacent active region. Standard flare loops from Eruption 1 developed over Eruption-2's flux rope and enclosed filament, but these overarching new loops were unable to confine that flux rope/filament. Eruption-1's flare loops, from both TW reconnection and standard-flare-model internal reconnection, were much cooler than Eruption-2's flare loops (GOES thermal temperatures of ~9 MK compared to ~14 MK). This eruption sequence produced a strong solar energetic particle (SEP) event (10 MeV protons, >10^3 pfu for 43 hrs), apparently starting when Eruption-2's CME blasted through Eruption-1's CME at 5---10 R_s. This occurred because the two CMEs originated in close proximity and in close time sequence: Eruption-1's fast rise started soon after the TW reconnection; the lid removal by Eruption-1's ejection triggered the slow onset of Eruption 2; and Eruption-2's CME, which started ~1 hr later, was three times faster than Eruption-1's CME. Title: Magnetic structure of sites of braiding in Hi-C active region Authors: Tiwari, Sanjiv Kumar; Alexander, Caroline; Winebarger, Amy R.; Moore, Ronald L. Bibcode: 2014AAS...22440904T Altcode: High-resolution Coronal Imager (Hi-C) observations of an active region (AR) corona, at a spatial resolution of 0.2 arcsec, have offered the first direct evidence of field lines braiding, which could deliver sufficient energy to heat the AR corona by current dissipation via magnetic reconnection, a proposal given by Parker three decades ago. The energy required to heat the corona must be transported from the photosphere along the field lines. The mechanism that drives the energy transport to the corona is not yet fully understood.To investigate simultaneous magnetic and intensity structure in and around the AR in detail, we use SDO/HMI+AIA data of + / - 2 hours around the 5 minute Hi-C flight. In the case of the QS, work done by convection/granulation on the inter-granular feet of the coronal field lines probably translates into the heat observed in the corona. In the case of the AR, as here, there could be flux emergence, cancellation/submergence, or shear flows generating large stress and tension in coronal field loops which is released as heat in the corona. However, to the best of our knowledge, there is no observational evidence available to these processes. We investigate the changes taking place in the photospheric feet of the magnetic field involved with brightenings in the Hi-C AR corona. Using HMI 45s magnetograms of four hours we find that, out of the two Hi-C sub-regions where the braiding of field lines were recently detected, flux emergence takes place in one region and flux cancellation in the other. The field in these sub-regions are highly sheared and have apparent high speed plasma flows at their feet. Therefore, shearing flows plausibly power much of the coronal and transition region heating in these areas of the AR. In addition, the presence of large flux emergence/cancellation strongly suggests that the work done by these processes on the pre-existing field also drives much of the observed heating.For this work, SKT and CEA were supported by an appointment to the NASA Postdoctoral Program at the NASA Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA, and AW and RLM were supported by funding from the Living With a Star Targeted Research and Technology Program of the Heliophysics Division of NASA's Science Mission Directorate. Title: Magnetic Untwisting in Jets that Go into the Outer Solar Corona in Polar Coronal Holes Authors: Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David Bibcode: 2014AAS...22440803M Altcode: We present results from a study of 14 jets that were observed in SDO/AIA EUV movies to erupt in the Sun’s polar coronal holes. These jets were similar to the many other jets that erupt in coronal holes, but reached higher than the vast majority, high enough to be observed in the outer corona beyond 2 solar radii from Sun center by the SOHO/LASCO/C2 coronagraph. We illustrate the characteristic structure and motion of these high-reaching jets by showing observations of two representative jets. We find that (1) the speed of the jet front from the base of the corona out to 2-3 solar radii is typically several times the sound speed in jets in coronal holes, (2) each high-reaching jet displays unusually large rotation about its axis (spin) as it erupts, and (3) in the outer corona, many jets display lateral swaying and bending of the jet axis with an amplitude of a few degrees and a period of order 1 hour. From these observations we infer that these jets are magnetically driven, propose that the driver is a magnetic-untwisting wave that is basically a large-amplitude (non-linear) torsional Alfven wave that is put into the open magnetic field in the jet by interchange reconnection as the jet erupts, and estimate that the magnetic-untwisting wave loses most of its energy before reaching the outer corona. These observations of high-reaching coronal jets suggest that the torsional magnetic waves observed in Type-II spicules can similarly dissipate in the corona and thereby power much of the coronal heating in coronal holes and quiet regions. This work is funded by the NASA/SMD Heliophysics Division’s Living With a Star Targeted Research & Technology Program. Title: Search for Invisible Decays of a Higgs Boson Produced in Association with a Z Boson in ATLAS Authors: Aad, G.; Abajyan, T.; Abbott, B.; Abdallah, J.; Abdel Khalek, S.; Abdinov, O.; Aben, R.; Abi, B.; Abolins, M.; Abouzeid, O. S.; Abramowicz, H.; Abreu, H.; Abulaiti, Y.; Acharya, B. S.; Adamczyk, L.; Adams, D. L.; Addy, T. N.; Adelman, J.; Adomeit, S.; Adye, T.; Aefsky, S.; Agatonovic-Jovin, T.; Aguilar-Saavedra, J. A.; Agustoni, M.; Ahlen, S. P.; Ahmad, A.; Ahmadov, F.; Aielli, G.; Åkesson, T. P. A.; Akimoto, G.; Akimov, A. V.; Alam, M. A.; Albert, J.; Albrand, S.; Alconada Verzini, M. J.; Aleksa, M.; Aleksandrov, I. N.; Alessandria, F.; Alexa, C.; Alexander, G.; Alexandre, G.; Alexopoulos, T.; Alhroob, M.; Alimonti, G.; Alio, L.; Alison, J.; Allbrooke, B. M. M.; Allison, L. J.; Allport, P. P.; Allwood-Spiers, S. E.; Almond, J.; Aloisio, A.; Alon, R.; Alonso, A.; Alonso, F.; Altheimer, A.; Alvarez Gonzalez, B.; Alviggi, M. G.; Amako, K.; Amaral Coutinho, Y.; Amelung, C.; Ammosov, V. V.; Amor Dos Santos, S. P.; Amorim, A.; Amoroso, S.; Amram, N.; Amundsen, G.; Anastopoulos, C.; Ancu, L. S.; Andari, N.; Andeen, T.; Anders, C. F.; Anders, G.; Anderson, K. J.; Andreazza, A.; Andrei, V.; Anduaga, X. S.; Angelidakis, S.; Anger, P.; Angerami, A.; Anghinolfi, F.; Anisenkov, A. V.; Anjos, N.; Annovi, A.; Antonaki, A.; Antonelli, M.; Antonov, A.; Antos, J.; Anulli, F.; Aoki, M.; Aperio Bella, L.; Apolle, R.; Arabidze, G.; Aracena, I.; Arai, Y.; Arce, A. T. H.; Arguin, J. -F.; Argyropoulos, S.; Arik, E.; Arik, M.; Armbruster, A. J.; Arnaez, O.; Arnal, V.; Arslan, O.; Artamonov, A.; Artoni, G.; Asai, S.; Asbah, N.; Ask, S.; Åsman, B.; Asquith, L.; Assamagan, K.; Astalos, R.; Astbury, A.; Atkinson, M.; Atlay, N. B.; Auerbach, B.; Auge, E.; Augsten, K.; Aurousseau, M.; Avolio, G.; Azuelos, G.; Azuma, Y.; Baak, M. A.; Bacci, C.; Bach, A. M.; Bachacou, H.; Bachas, K.; Backes, M.; Backhaus, M.; Backus Mayes, J.; Badescu, E.; Bagiacchi, P.; Bagnaia, P.; Bai, Y.; Bailey, D. C.; Bain, T.; Baines, J. T.; Baker, O. K.; Baker, S.; Balek, P.; Balli, F.; Banas, E.; Banerjee, Sw.; Banfi, D.; Bangert, A.; Bansal, V.; Bansil, H. S.; Barak, L.; Baranov, S. P.; Barber, T.; Barberio, E. L.; Barberis, D.; Barbero, M.; Barillari, T.; Barisonzi, M.; Barklow, T.; Barlow, N.; Barnett, B. M.; Barnett, R. M.; Baroncelli, A.; Barone, G.; Barr, A. J.; Barreiro, F.; Barreiro Guimarães da Costa, J.; Bartoldus, R.; Barton, A. E.; Bartos, P.; Bartsch, V.; Bassalat, A.; Basye, A.; Bates, R. L.; Batkova, L.; Batley, J. 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M.; Trincaz-Duvoid, S.; Tripiana, M. F.; Triplett, N.; Trischuk, W.; Trocmé, B.; Troncon, C.; Trottier-McDonald, M.; Trovatelli, M.; True, P.; Trzebinski, M.; Trzupek, A.; Tsarouchas, C.; Tseng, J. C. -L.; Tsiareshka, P. V.; Tsionou, D.; Tsipolitis, G.; Tsirintanis, N.; Tsiskaridze, S.; Tsiskaridze, V.; Tskhadadze, E. G.; Tsukerman, I. I.; Tsulaia, V.; Tsung, J. -W.; Tsuno, S.; Tsybychev, D.; Tua, A.; Tudorache, A.; Tudorache, V.; Tuna, A. N.; Tupputi, S. A.; Turchikhin, S.; Turecek, D.; Turk Cakir, I.; Turra, R.; Tuts, P. M.; Tykhonov, A.; Tylmad, M.; Tyndel, M.; Uchida, K.; Ueda, I.; Ueno, R.; Ughetto, M.; Ugland, M.; Uhlenbrock, M.; Ukegawa, F.; Unal, G.; Undrus, A.; Unel, G.; Ungaro, F. C.; Unno, Y.; Urbaniec, D.; Urquijo, P.; Usai, G.; Usanova, A.; Vacavant, L.; Vacek, V.; Vachon, B.; Valencic, N.; Valentinetti, S.; Valero, A.; Valery, L.; Valkar, S.; Valladolid Gallego, E.; Vallecorsa, S.; Valls Ferrer, J. A.; van Berg, R.; van der Deijl, P. C.; van der Geer, R.; van der Graaf, H.; van der Leeuw, R.; van der Ster, D.; van Eldik, N.; van Gemmeren, P.; van Nieuwkoop, J.; van Vulpen, I.; van Woerden, M. C.; Vanadia, M.; Vandelli, W.; Vaniachine, A.; Vankov, P.; Vannucci, F.; Vardanyan, G.; Vari, R.; Varnes, E. W.; Varol, T.; Varouchas, D.; Vartapetian, A.; Varvell, K. E.; Vassilakopoulos, V. I.; Vazeille, F.; Vazquez Schroeder, T.; Veatch, J.; Veloso, F.; Veneziano, S.; Ventura, A.; Ventura, D.; Venturi, M.; Venturi, N.; Venturini, A.; Vercesi, V.; Verducci, M.; Verkerke, W.; Vermeulen, J. C.; Vest, A.; Vetterli, M. C.; Viazlo, O.; Vichou, I.; Vickey, T.; Vickey Boeriu, O. E.; Viehhauser, G. H. A.; Viel, S.; Vigne, R.; Villa, M.; Villaplana Perez, M.; Vilucchi, E.; Vincter, M. G.; Vinogradov, V. B.; Virzi, J.; Vitells, O.; Vivarelli, I.; Vives Vaque, F.; Vlachos, S.; Vladoiu, D.; Vlasak, M.; Vogel, A.; Vokac, P.; Volpi, G.; Volpi, M.; Volpini, G.; von der Schmitt, H.; von Radziewski, H.; von Toerne, E.; Vorobel, V.; Vos, M.; Voss, R.; Vossebeld, J. H.; Vranjes, N.; Vranjes Milosavljevic, M.; Vrba, V.; Vreeswijk, M.; Vu Anh, T.; Vuillermet, R.; Vukotic, I.; Vykydal, Z.; Wagner, W.; Wagner, P.; Wahrmund, S.; Wakabayashi, J.; Walder, J.; Walker, R.; Walkowiak, W.; Wall, R.; Waller, P.; Walsh, B.; Wang, C.; Wang, H.; Wang, H.; Wang, J.; Wang, J.; Wang, K.; Wang, R.; Wang, S. M.; Wang, T.; Wang, X.; Warburton, A.; Ward, C. P.; Wardrope, D. R.; Warsinsky, M.; Washbrook, A.; Wasicki, C.; Watanabe, I.; Watkins, P. M.; Watson, A. T.; Watson, I. J.; Watson, M. F.; Watts, G.; Watts, S.; Waugh, A. T.; Waugh, B. M.; Webb, S.; Weber, M. S.; Weber, S. W.; Webster, J. S.; Weidberg, A. R.; Weigell, P.; Weingarten, J.; Weiser, C.; Weits, H.; Wells, P. S.; Wenaus, T.; Wendland, D.; Weng, Z.; Wengler, T.; Wenig, S.; Wermes, N.; Werner, M.; Werner, P.; Wessels, M.; Wetter, J.; Whalen, K.; White, A.; White, M. J.; White, R.; White, S.; Whiteson, D.; Whittington, D.; Wicke, D.; Wickens, F. J.; Wiedenmann, W.; Wielers, M.; Wienemann, P.; Wiglesworth, C.; Wiik-Fuchs, L. A. M.; Wijeratne, P. A.; Wildauer, A.; Wildt, M. A.; Wilkens, H. G.; Will, J. Z.; Williams, H. H.; Williams, S.; Willis, W.; Willocq, S.; Wilson, J. A.; Wilson, A.; Wingerter-Seez, I.; Winkelmann, S.; Winklmeier, F.; Wittgen, M.; Wittig, T.; Wittkowski, J.; Wollstadt, S. J.; Wolter, M. W.; Wolters, H.; Wong, W. C.; Wosiek, B. K.; Wotschack, J.; Woudstra, M. J.; Wozniak, K. W.; Wraight, K.; Wright, M.; Wu, S. L.; Wu, X.; Wu, Y.; Wulf, E.; Wyatt, T. R.; Wynne, B. M.; Xella, S.; Xiao, M.; Xu, D.; Xu, L.; Yabsley, B.; Yacoob, S.; Yamada, M.; Yamaguchi, H.; Yamaguchi, Y.; Yamamoto, A.; Yamamoto, K.; Yamamoto, S.; Yamamura, T.; Yamanaka, T.; Yamauchi, K.; Yamazaki, Y.; Yan, Z.; Yang, H.; Yang, H.; Yang, U. K.; Yang, Y.; Yanush, S.; Yao, L.; Yasu, Y.; Yatsenko, E.; Yau Wong, K. H.; Ye, J.; Ye, S.; Yen, A. L.; Yildirim, E.; Yilmaz, M.; Yoosoofmiya, R.; Yorita, K.; Yoshida, R.; Yoshihara, K.; Young, C.; Young, C. J. S.; Youssef, S.; Yu, D. R.; Yu, J.; Yu, J. M.; Yu, J.; Yuan, L.; Yurkewicz, A.; Zabinski, B.; Zaidan, R.; Zaitsev, A. M.; Zaman, A.; Zambito, S.; Zanello, L.; Zanzi, D.; Zaytsev, A.; Zeitnitz, C.; Zeman, M.; Zemla, A.; Zengel, K.; Zenin, O.; Ženiš, T.; Zerwas, D.; Zevi Della Porta, G.; Zhang, D.; Zhang, H.; Zhang, J.; Zhang, L.; Zhang, X.; Zhang, Z.; Zhao, Z.; Zhemchugov, A.; Zhong, J.; Zhou, B.; Zhou, L.; Zhou, N.; Zhu, C. G.; Zhu, H.; Zhu, J.; Zhu, Y.; Zhuang, X.; Zibell, A.; Zieminska, D.; Zimine, N. I.; Zimmermann, C.; Zimmermann, R.; Zimmermann, S.; Zimmermann, S.; Zinonos, Z.; Ziolkowski, M.; Zitoun, R.; Zobernig, G.; Zoccoli, A.; Zur Nedden, M.; Zurzolo, G.; Zutshi, V.; Zwalinski, L.; Atlas Collaboration Bibcode: 2014PhRvL.112t1802A Altcode: 2014arXiv1402.3244A A search for evidence of invisible-particle decay modes of a Higgs boson produced in association with a Z boson at the Large Hadron Collider is presented. No deviation from the standard model expectation is observed in 4.5 fb-1 (20.3 fb-1) of 7 (8) TeV pp collision data collected by the ATLAS experiment. Assuming the standard model rate for ZH production, an upper limit of 75%, at the 95% confidence level is set on the branching ratio to invisible-particle decay modes of the Higgs boson at a mass of 125.5 GeV. The limit on the branching ratio is also interpreted in terms of an upper limit on the allowed dark matter-nucleon scattering cross section within a Higgs-portal dark matter scenario. Within the constraints of such a scenario, the results presented in this Letter provide the strongest available limits for low-mass dark matter candidates. Limits are also set on an additional neutral Higgs boson, in the mass range 110<mH<400 GeV, produced in association with a Z boson and decaying to invisible particles. Title: A Small-scale Eruption Leading to a Blowout Macrospicule Jet in an On-disk Coronal Hole Authors: Adams, Mitzi; Sterling, Alphonse C.; Moore, Ronald L.; Gary, G. Allen Bibcode: 2014ApJ...783...11A Altcode: We examine the three-dimensional magnetic structure and dynamics of a solar EUV-macrospicule jet that occurred on 2011 February 27 in an on-disk coronal hole. The observations are from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) and the SDO Helioseismic and Magnetic Imager (HMI). The observations reveal that in this event, closed-field-carrying cool absorbing plasma, as in an erupting mini-filament, erupted and opened, forming a blowout jet. Contrary to some jet models, there was no substantial recently emerged, closed, bipolar-magnetic field in the base of the jet. Instead, over several hours, flux convergence and cancellation at the polarity inversion line inside an evolved arcade in the base apparently destabilized the entire arcade, including its cool-plasma-carrying core field, to undergo a blowout eruption in the manner of many standard-sized, arcade-blowout eruptions that produce a flare and coronal mass ejection. Internal reconnection made bright "flare" loops over the polarity inversion line inside the blowing-out arcade field, and external reconnection of the blowing-out arcade field with an ambient open field made longer and dimmer EUV loops on the outside of the blowing-out arcade. That the loops made by the external reconnection were much larger than the loops made by the internal reconnection makes this event a new variety of blowout jet, a variety not recognized in previous observations and models of blowout jets. Title: Search for Dark Matter in Events with a Hadronically Decaying W or Z Boson and Missing Transverse Momentum in pp Collisions at √s =8 TeV with the ATLAS Detector Authors: Aad, G.; Abajyan, T.; Abbott, B.; Abdallah, J.; Abdel Khalek, S.; Abdinov, O.; Aben, R.; Abi, B.; Abolins, M.; Abouzeid, O. S.; Abramowicz, H.; Abreu, H.; Abulaiti, Y.; Acharya, B. S.; Adamczyk, L.; Adams, D. L.; Addy, T. N.; Adelman, J.; Adomeit, S.; Adye, T.; Aefsky, S.; Agatonovic-Jovin, T.; Aguilar-Saavedra, J. A.; Agustoni, M.; Ahlen, S. P.; Ahmad, A.; Ahmadov, F.; Ahsan, M.; Aielli, G.; Åkesson, T. P. A.; Akimoto, G.; Akimov, A. V.; Alam, M. A.; Albert, J.; Albrand, S.; Alconada Verzini, M. J.; Aleksa, M.; Aleksandrov, I. N.; Alessandria, F.; Alexa, C.; Alexander, G.; Alexandre, G.; Alexopoulos, T.; Alhroob, M.; Aliev, M.; Alimonti, G.; Alio, L.; Alison, J.; Allbrooke, B. M. M.; Allison, L. J.; Allport, P. P.; Allwood-Spiers, S. E.; Almond, J.; Aloisio, A.; Alon, R.; Alonso, A.; Alonso, F.; Altheimer, A.; Alvarez Gonzalez, B.; Alviggi, M. G.; Amako, K.; Amaral Coutinho, Y.; Amelung, C.; Ammosov, V. V.; Amor Dos Santos, S. P.; Amorim, A.; Amoroso, S.; Amram, N.; Amundsen, G.; Anastopoulos, C.; Ancu, L. S.; Andari, N.; Andeen, T.; Anders, C. F.; Anders, G.; Anderson, K. J.; Andreazza, A.; Andrei, V.; Anduaga, X. S.; Angelidakis, S.; Anger, P.; Angerami, A.; Anghinolfi, F.; Anisenkov, A. V.; Anjos, N.; Annovi, A.; Antonaki, A.; Antonelli, M.; Antonov, A.; Antos, J.; Anulli, F.; Aoki, M.; Aperio Bella, L.; Apolle, R.; Arabidze, G.; Aracena, I.; Arai, Y.; Arce, A. T. H.; Arfaoui, S.; Arguin, J. -F.; Argyropoulos, S.; Arik, E.; Arik, M.; Armbruster, A. J.; Arnaez, O.; Arnal, V.; Arslan, O.; Artamonov, A.; Artoni, G.; Asai, S.; Asbah, N.; Ask, S.; Åsman, B.; Asquith, L.; Assamagan, K.; Astalos, R.; Astbury, A.; Atkinson, M.; Atlay, N. B.; Auerbach, B.; Auge, E.; Augsten, K.; Aurousseau, M.; Avolio, G.; Azuelos, G.; Azuma, Y.; Baak, M. A.; Bacci, C.; Bach, A. M.; Bachacou, H.; Bachas, K.; Backes, M.; Backhaus, M.; Backus Mayes, J.; Badescu, E.; Bagiacchi, P.; Bagnaia, P.; Bai, Y.; Bailey, D. C.; Bain, T.; Baines, J. T.; Baker, O. K.; Baker, S.; Balek, P.; Balli, F.; Banas, E.; Banerjee, Sw.; Banfi, D.; Bangert, A.; Bansal, V.; Bansil, H. S.; Barak, L.; Baranov, S. P.; Barber, T.; Barberio, E. L.; Barberis, D.; Barbero, M.; Bardin, D. Y.; Barillari, T.; Barisonzi, M.; Barklow, T.; Barlow, N.; Barnett, B. M.; Barnett, R. M.; Baroncelli, A.; Barone, G.; Barr, A. J.; Barreiro, F.; Barreiro Guimarães da Costa, J.; Bartoldus, R.; Barton, A. E.; Bartsch, V.; Bassalat, A.; Basye, A.; Bates, R. L.; Batkova, L.; Batley, J. R.; Battistin, M.; Bauer, F.; Bawa, H. S.; Beau, T.; Beauchemin, P. H.; Beccherle, R.; Bechtle, P.; Beck, H. P.; Becker, K.; Becker, S.; Beckingham, M.; Beddall, A. J.; Beddall, A.; Bedikian, S.; Bednyakov, V. A.; Bee, C. P.; Beemster, L. J.; Beermann, T. A.; Begel, M.; Behr, K.; Belanger-Champagne, C.; Bell, P. J.; Bell, W. H.; Bella, G.; Bellagamba, L.; Bellerive, A.; Bellomo, M.; Belloni, A.; Beloborodova, O. L.; Belotskiy, K.; Beltramello, O.; Benary, O.; Benchekroun, D.; Bendtz, K.; Benekos, N.; Benhammou, Y.; Benhar Noccioli, E.; Benitez Garcia, J. A.; Benjamin, D. P.; Bensinger, J. R.; Benslama, K.; Bentvelsen, S.; Berge, D.; Bergeaas Kuutmann, E.; Berger, N.; Berghaus, F.; Berglund, E.; Beringer, J.; Bernard, C.; Bernat, P.; Bernhard, R.; Bernius, C.; Bernlochner, F. U.; Berry, T.; Berta, P.; Bertella, C.; Bertolucci, F.; Besana, M. I.; Besjes, G. J.; Bessidskaia, O.; Besson, N.; Bethke, S.; Bhimji, W.; Bianchi, R. M.; Bianchini, L.; Bianco, M.; Biebel, O.; Bieniek, S. P.; Bierwagen, K.; Biesiada, J.; Biglietti, M.; Bilbao de Mendizabal, J.; Bilokon, H.; Bindi, M.; Binet, S.; Bingul, A.; Bini, C.; Bittner, B.; Black, C. W.; Black, J. E.; Black, K. M.; Blackburn, D.; Blair, R. E.; Blanchard, J. -B.; Blazek, T.; Bloch, I.; Blocker, C.; Blocki, J.; Blum, W.; Blumenschein, U.; Bobbink, G. J.; Bobrovnikov, V. S.; Bocchetta, S. S.; Bocci, A.; Boddy, C. R.; Boehler, M.; Boek, J.; Boek, T. T.; Boelaert, N.; Bogaerts, J. A.; Bogdanchikov, A. G.; Bogouch, A.; Bohm, C.; Bohm, J.; Boisvert, V.; Bold, T.; Boldea, V.; Boldyrev, A. S.; Bolnet, N. M.; Bomben, M.; Bona, M.; Boonekamp, M.; Bordoni, S.; Borer, C.; Borisov, A.; Borissov, G.; Borri, M.; Borroni, S.; Bortfeldt, J.; Bortolotto, V.; Bos, K.; Boscherini, D.; Bosman, M.; Boterenbrood, H.; Bouchami, J.; Boudreau, J.; Bouhova-Thacker, E. V.; Boumediene, D.; Bourdarios, C.; Bousson, N.; Boutouil, S.; Boveia, A.; Boyd, J.; Boyko, I. R.; Bozovic-Jelisavcic, I.; Bracinik, J.; Branchini, P.; Brandt, A.; Brandt, G.; Brandt, O.; Bratzler, U.; Brau, B.; Brau, J. E.; Braun, H. M.; Brazzale, S. F.; Brelier, B.; Brendlinger, K.; Brenner, R.; Bressler, S.; Bristow, T. M.; Britton, D.; Brochu, F. M.; Brock, I.; Brock, R.; Broggi, F.; Bromberg, C.; Bronner, J.; Brooijmans, G.; Brooks, T.; Brooks, W. K.; Brosamer, J.; Brost, E.; Brown, G.; Brown, J.; Bruckman de Renstrom, P. A.; Bruncko, D.; Bruneliere, R.; Brunet, S.; Bruni, A.; Bruni, G.; Bruschi, M.; Bryngemark, L.; Buanes, T.; Buat, Q.; Bucci, F.; Buchanan, J.; Buchholz, P.; Buckingham, R. M.; Buckley, A. G.; Buda, S. I.; Budagov, I. A.; Budick, B.; Buehrer, F.; Bugge, L.; Bulekov, O.; Bundock, A. C.; Bunse, M.; Burckhart, H.; Burdin, S.; Burgess, T.; Burke, S.; Burmeister, I.; Busato, E.; Büscher, V.; Bussey, P.; Buszello, C. P.; Butler, B.; Butler, J. M.; Butt, A. I.; Buttar, C. M.; Butterworth, J. M.; Buttinger, W.; Buzatu, A.; Byszewski, M.; Cabrera Urbán, S.; Caforio, D.; Cakir, O.; Calafiura, P.; Calderini, G.; Calfayan, P.; Calkins, R.; Caloba, L. P.; Caloi, R.; Calvet, D.; Calvet, S.; Camacho Toro, R.; Camarri, P.; Cameron, D.; Caminada, L. M.; Caminal Armadans, R.; Campana, S.; Campanelli, M.; Canale, V.; Canelli, F.; Canepa, A.; Cantero, J.; Cantrill, R.; Cao, T.; Capeans Garrido, M. D. M.; Caprini, I.; Caprini, M.; Capua, M.; Caputo, R.; Cardarelli, R.; Carli, T.; Carlino, G.; Carminati, L.; Caron, S.; Carquin, E.; Carrillo-Montoya, G. D.; Carter, A. A.; Carter, J. R.; Carvalho, J.; Casadei, D.; Casado, M. P.; Caso, C.; Castaneda-Miranda, E.; Castelli, A.; Castillo Gimenez, V.; Castro, N. F.; Catastini, P.; Catinaccio, A.; Catmore, J. R.; Cattai, A.; Cattani, G.; Caughron, S.; Cavaliere, V.; Cavalli, D.; Cavalli-Sforza, M.; Cavasinni, V.; Ceradini, F.; Cerio, B.; Cerny, K.; Cerqueira, A. S.; Cerri, A.; Cerrito, L.; Cerutti, F.; Cervelli, A.; Cetin, S. A.; Chafaq, A.; Chakraborty, D.; Chalupkova, I.; Chan, K.; Chang, P.; Chapleau, B.; Chapman, J. D.; Chapman, J. W.; Charfeddine, D.; Charlton, D. G.; Chavda, V.; Chavez Barajas, C. A.; Cheatham, S.; Chekanov, S.; Chekulaev, S. V.; Chelkov, G. A.; Chelstowska, M. A.; Chen, C.; Chen, H.; Chen, K.; Chen, S.; Chen, X.; Chen, Y.; Cheng, Y.; Cheplakov, A.; Cherkaoui El Moursli, R.; Chernyatin, V.; Cheu, E.; Chevalier, L.; Chiarella, V.; Chiefari, G.; Childers, J. T.; Chilingarov, A.; Chiodini, G.; Chisholm, A. S.; Chislett, R. T.; Chitan, A.; Chizhov, M. V.; Choudalakis, G.; Chouridou, S.; Chow, B. K. B.; Christidi, I. A.; Chromek-Burckhart, D.; Chu, M. L.; Chudoba, J.; Ciapetti, G.; Ciftci, A. K.; Ciftci, R.; Cinca, D.; Cindro, V.; Ciocio, A.; Cirilli, M.; Cirkovic, P.; Citron, Z. H.; Citterio, M.; Ciubancan, M.; Clark, A.; Clark, P. J.; Clarke, R. N.; Clemens, J. C.; Clement, B.; Clement, C.; Coadou, Y.; Cobal, M.; Coccaro, A.; Cochran, J.; Coelli, S.; Coffey, L.; Cogan, J. 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I.; Vazeille, F.; Vazquez Schroeder, T.; Veatch, J.; Veloso, F.; Veneziano, S.; Ventura, A.; Ventura, D.; Venturi, M.; Venturi, N.; Vercesi, V.; Verducci, M.; Verkerke, W.; Vermeulen, J. C.; Vest, A.; Vetterli, M. C.; Viazlo, O.; Vichou, I.; Vickey, T.; Vickey Boeriu, O. E.; Viehhauser, G. H. A.; Viel, S.; Vigne, R.; Villa, M.; Villaplana Perez, M.; Vilucchi, E.; Vincter, M. G.; Vinogradov, V. B.; Virzi, J.; Vitells, O.; Viti, M.; Vivarelli, I.; Vives Vaque, F.; Vlachos, S.; Vladoiu, D.; Vlasak, M.; Vogel, A.; Vokac, P.; Volpi, G.; Volpi, M.; Volpini, G.; von der Schmitt, H.; von Radziewski, H.; von Toerne, E.; Vorobel, V.; Vos, M.; Voss, R.; Vossebeld, J. H.; Vranjes, N.; Vranjes Milosavljevic, M.; Vrba, V.; Vreeswijk, M.; Vu Anh, T.; Vuillermet, R.; Vukotic, I.; Vykydal, Z.; Wagner, W.; Wagner, P.; Wahrmund, S.; Wakabayashi, J.; Walch, S.; Walder, J.; Walker, R.; Walkowiak, W.; Wall, R.; Waller, P.; Walsh, B.; Wang, C.; Wang, H.; Wang, H.; Wang, J.; Wang, J.; Wang, K.; Wang, R.; Wang, S. M.; Wang, T.; Wang, X.; Warburton, A.; Ward, C. P.; Wardrope, D. R.; Warsinsky, M.; Washbrook, A.; Wasicki, C.; Watanabe, I.; Watkins, P. M.; Watson, A. T.; Watson, I. J.; Watson, M. F.; Watts, G.; Watts, S.; Waugh, A. T.; Waugh, B. M.; Webb, S.; Weber, M. S.; Weber, S. W.; Webster, J. S.; Weidberg, A. R.; Weigell, P.; Weingarten, J.; Weiser, C.; Weits, H.; Wells, P. S.; Wenaus, T.; Wendland, D.; Weng, Z.; Wengler, T.; Wenig, S.; Wermes, N.; Werner, M.; Werner, P.; Wessels, M.; Wetter, J.; Whalen, K.; White, A.; White, M. J.; White, R.; White, S.; Whiteson, D.; Whittington, D.; Wicke, D.; Wickens, F. J.; Wiedenmann, W.; Wielers, M.; Wienemann, P.; Wiglesworth, C.; Wiik-Fuchs, L. A. M.; Wijeratne, P. A.; Wildauer, A.; Wildt, M. A.; Wilhelm, I.; Wilkens, H. G.; Will, J. Z.; Williams, E.; Williams, H. H.; Williams, S.; Willis, W.; Willocq, S.; Wilson, J. A.; Wilson, A.; Wingerter-Seez, I.; Winkelmann, S.; Winklmeier, F.; Wittgen, M.; Wittig, T.; Wittkowski, J.; Wollstadt, S. J.; Wolter, M. W.; Wolters, H.; Wong, W. C.; Wosiek, B. K.; Wotschack, J.; Woudstra, M. J.; Wozniak, K. W.; Wraight, K.; Wright, M.; Wu, S. L.; Wu, X.; Wu, Y.; Wulf, E.; Wyatt, T. R.; Wynne, B. M.; Xella, S.; Xiao, M.; Xu, C.; Xu, D.; Xu, L.; Yabsley, B.; Yacoob, S.; Yamada, M.; Yamaguchi, H.; Yamaguchi, Y.; Yamamoto, A.; Yamamoto, K.; Yamamoto, S.; Yamamura, T.; Yamanaka, T.; Yamauchi, K.; Yamazaki, Y.; Yan, Z.; Yang, H.; Yang, H.; Yang, U. K.; Yang, Y.; Yang, Z.; Yanush, S.; Yao, L.; Yasu, Y.; Yatsenko, E.; Yau Wong, K. H.; Ye, J.; Ye, S.; Yen, A. L.; Yildirim, E.; Yilmaz, M.; Yoosoofmiya, R.; Yorita, K.; Yoshida, R.; Yoshihara, K.; Young, C.; Young, C. J. S.; Youssef, S.; Yu, D. R.; Yu, J.; Yu, J.; Yuan, L.; Yurkewicz, A.; Zabinski, B.; Zaidan, R.; Zaitsev, A. M.; Zaman, A.; Zambito, S.; Zanello, L.; Zanzi, D.; Zaytsev, A.; Zeitnitz, C.; Zeman, M.; Zemla, A.; Zenin, O.; Ženiš, T.; Zerwas, D.; Zevi Della Porta, G.; Zhang, D.; Zhang, H.; Zhang, J.; Zhang, L.; Zhang, X.; Zhang, Z.; Zhao, Z.; Zhemchugov, A.; Zhong, J.; Zhou, B.; Zhou, L.; Zhou, N.; Zhu, C. G.; Zhu, H.; Zhu, J.; Zhu, Y.; Zhuang, X.; Zibell, A.; Zieminska, D.; Zimin, N. I.; Zimmermann, C.; Zimmermann, R.; Zimmermann, S.; Zimmermann, S.; Zinonos, Z.; Ziolkowski, M.; Zitoun, R.; Živković, L.; Zobernig, G.; Zoccoli, A.; Zur Nedden, M.; Zurzolo, G.; Zutshi, V.; Zwalinski, L.; Atlas Collaboration Bibcode: 2014PhRvL.112d1802A Altcode: A search is presented for dark matter pair production in association with a W or Z boson in pp collisions representing 20.3 fb-1 of integrated luminosity at √s =8 TeV using data recorded with the ATLAS detector at the Large Hadron Collider. Events with a hadronic jet with the jet mass consistent with a W or Z boson, and with large missing transverse momentum are analyzed. The data are consistent with the standard model expectations. Limits are set on the mass scale in effective field theories that describe the interaction of dark matter and standard model particles, and on the cross section of Higgs production and decay to invisible particles. In addition, cross section limits on the anomalous production of W or Z bosons with large missing transverse momentum are set in two fiducial regions. Title: Einar Tandberg-Hanssen Authors: Schmieder, Brigitte; Pecker, Jean-Claude; Gary, Allen; Wu, S. T.; Moore, Ronald; Biesmann, Else Bibcode: 2014IAUS..300....4S Altcode: I would like to report first on the scientific career of Einar Tandberg-Hanssen: how he became a Solar Physicist particularly interested in prominences. In the second part of my talk I will show what he brought to the French community from the science perspective. Title: Evidence for Solar Tether-cutting Magnetic Reconnection from Coronal Field Extrapolations Authors: Liu, Chang; Deng, Na; Lee, Jeongwoo; Wiegelmann, Thomas; Moore, Ronald L.; Wang, Haimin Bibcode: 2013ApJ...778L..36L Altcode: 2013arXiv1310.5098L Magnetic reconnection is one of the primary mechanisms for triggering solar eruptive events, but direct observation of this rapid process has been a challenge. In this Letter, using a nonlinear force-free field (NLFFF) extrapolation technique, we present a visualization of field line connectivity changes resulting from tether-cutting reconnection over about 30 minutes during the 2011 February 13 M6.6 flare in NOAA AR 11158. Evidence for the tether-cutting reconnection was first collected through multiwavelength observations and then by analysis of the field lines traced from positions of four conspicuous flare 1700 Å footpoints observed at the event onset. Right before the flare, the four footpoints are located very close to the regions of local maxima of the magnetic twist index. In particular, the field lines from the inner two footpoints form two strongly twisted flux bundles (up to ~1.2 turns), which shear past each other and reach out close to the outer two footpoints, respectively. Immediately after the flare, the twist index of regions around the footpoints diminishes greatly and the above field lines become low-lying and less twisted (lsim0.6 turns), overarched by loops linking the two flare ribbons formed later. About 10% of the flux (~3 × 1019 Mx) from the inner footpoints undergoes a footpoint exchange. This portion of flux originates from the edge regions of the inner footpoints that are brightened first. These rapid changes of magnetic field connectivity inferred from the NLFFF extrapolation are consistent with the tether-cutting magnetic reconnection model. Title: Detecting Nanoflare Heating Events in Subarcsecond Inter-moss Loops Using Hi-C Authors: Winebarger, Amy R.; Walsh, Robert W.; Moore, Ronald; De Pontieu, Bart; Hansteen, Viggo; Cirtain, Jonathan; Golub, Leon; Kobayashi, Ken; Korreck, Kelly; DeForest, Craig; Weber, Mark; Title, Alan; Kuzin, Sergey Bibcode: 2013ApJ...771...21W Altcode: The High-resolution Coronal Imager (Hi-C) flew aboard a NASA sounding rocket on 2012 July 11 and captured roughly 345 s of high-spatial and temporal resolution images of the solar corona in a narrowband 193 Å channel. In this paper, we analyze a set of rapidly evolving loops that appear in an inter-moss region. We select six loops that both appear in and fade out of the Hi-C images during the short flight. From the Hi-C data, we determine the size and lifetimes of the loops and characterize whether these loops appear simultaneously along their length or first appear at one footpoint before appearing at the other. Using co-aligned, co-temporal data from multiple channels of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory, we determine the temperature and density of the loops. We find the loops consist of cool (~105 K), dense (~1010 cm-3) plasma. Their required thermal energy and their observed evolution suggest they result from impulsive heating similar in magnitude to nanoflares. Comparisons with advanced numerical simulations indicate that such dense, cold and short-lived loops are a natural consequence of impulsive magnetic energy release by reconnection of braided magnetic field at low heights in the solar atmosphere. Title: Magnetic Untwisting in Most Solar X-Ray Jets Authors: Moore, Ronald L.; Sterling, A. C.; Falconer, D.; Robe, D. M. Bibcode: 2013SPD....4410304M Altcode: From 54 X-ray jets observed in the polar coronal holes by Hinode’s X-Ray Telescope (XRT) during coverage in movies from Solar Dynamic Observatory’s Atmospheric Imaging Assembly (AIA) taken in its He II 304 Å band at a cadence of 12 s, we have established a basic characteristic of solar X-ray jets: untwisting motion in the spire. In this presentation, we show the progression of few of these X-ray jets in XRT images and track their untwisting in AIA He II images. From their structure displayed in their XRT movies, 19 jets were evidently standard jets made by interchange reconnection of the magnetic-arcade base with ambient open field, 32 were evidently blowout jets made by blowout eruption of the base arcade, and 3 were of ambiguous form. As was anticipated from the >10,000 km span of the base arcade in most polar X-ray jets and from the disparity of standard jets and blowout jets in their magnetic production, few of the standard X-ray jets (3 of 19) but nearly all of the blowout X-ray jets (29 of 32) carried enough cool (T ~ 10^5 K) plasma to be seen in their He II movies. In the 32 X-ray jets that showed a cool component, the He II movies show 10-100 km/s untwisting motions about the axis of the spire in all 3 standard jets and in 26 of the 29 blowout jets. Evidently, the open magnetic field in nearly all blowout X-ray jets and probably in most standard X-ray jets carries transient twist. This twist apparently relaxes by propagating out along the open field as a torsional wave. High-resolution spectrograms and Dopplergrams have shown that most Type-II spicules have torsional motions of 10-30 km/s. Our observation of similar torsional motion in X-ray jets (1) strengthens the case for Type-II spicules being made in the same way as X-ray jets, by blowout eruption of a twisted magnetic arcade in the spicule base and/or by interchange reconnection of the twisted base arcade with the ambient open field, and hence (2) strengthens the case made by Moore et al (2011, ApJ, 731: L18) that the Sun's granule-size emerging magnetic bipoles, by making Type-II spicules, power the global corona and solar wind. This work was funded by NASA’s LWS TRT Program, NASA's Hinode Project, and NSF's REU Program. Title: A Small-Scale Filament Eruption Leading to a Blowout Macrospicule Jet in an On-Disk Coronal Hole Authors: Sterling, Alphonse C.; Adams, M.; Moore, R. L.; Tennant, A. F.; Gary, G. A. Bibcode: 2013SPD....44...17S Altcode: We observe an eruptive jet that occurred in an on-disk solar coronal hole, using EUV images from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA), supplemented by magnetic data from the SDO Helioseismic and Magnetic Imager (HMI). This jet is similar to features variously called macrospicules or erupting minifilaments. After an initial pre-eruptive phase, a concentration of absorbing, cool material in the AIA images moves with a substantially-horizontal motion toward a region of open magnetic field, and subsequently jets out along that vertical field. Prior to and during the jet's ~20 min lifetime, the magnetic flux integrated over the local region shows flux changes of < 20% of the background flux levels, with a time-averaged emergence rate of no more than <3 × 10^15 Mx/s in the neighborhood of the jet. Contrary to some jet models, there was no substantial recently-emerged bipolar field in the base of the jet. Instead, there was an established evolving magnetic arcade that held mini-filament-like cool plasma in its core field. We propose that subtle evolution of the magnetic flux in and around this arcade destabilized its core field, as in some standard-sized arcade blowout eruptions that produce a flare and CME following the slow rise of a standard-sized filament in the core of the arcade. Closed field carrying the cool plasma erupted into the open field and formed the blowout jet, evidently at least partly by interchange reconnection with the open field. Internal reconnection made compact bright "flare" loops inside the blowing-out arcade, while, on the outside, interchange reconnection made longer and dimmer EUV "crinkle" loops. That the loops made by the external reconnection were considerably larger than the loops made by the internal reconnection makes this event a new variety of blowout jet, a variety not recognized in previous observations and models of blowout jets. Title: The Cool Component and the Dichotomy, Lateral Expansion, and Axial Rotation of Solar X-Ray Jets Authors: Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David A.; Robe, Dominic Bibcode: 2013ApJ...769..134M Altcode: We present results from a study of 54 polar X-ray jets that were observed in coronal X-ray movies from the X-ray Telescope on Hinode and had simultaneous coverage in movies of the cooler transition region (T ~ 105 K) taken in the He II 304 Å band of the Atmospheric Imaging Assembly (AIA) on Solar Dynamics Observatory. These dual observations verify the standard-jet/blowout-jet dichotomy of polar X-ray jets previously found primarily from XRT movies alone. In accord with models of blowout jets and standard jets, the AIA 304 Å movies show a cool (T ~ 105 K) component in nearly all blowout X-ray jets and in a small minority of standard X-ray jets, obvious lateral expansion in blowout X-ray jets but none in standard X-ray jets, and obvious axial rotation in both blowout X-ray jets and standard X-ray jets. In our sample, the number of turns of axial rotation in the cool-component standard X-ray jets is typical of that in the blowout X-ray jets, suggesting that the closed bipolar magnetic field in the jet base has substantial twist not only in all blowout X-ray jets but also in many standard X-ray jets. We point out that our results for the dichotomy, lateral expansion, and axial rotation of X-ray jets add credence to published speculation that type-II spicules are miniature analogs of X-ray jets, are generated by granule-size emerging bipoles, and thereby carry enough energy to power the corona and solar wind. Title: Energy release in the solar corona from spatially resolved magnetic braids Authors: Cirtain, J. W.; Golub, L.; Winebarger, A. R.; de Pontieu, B.; Kobayashi, K.; Moore, R. L.; Walsh, R. W.; Korreck, K. E.; Weber, M.; McCauley, P.; Title, A.; Kuzin, S.; Deforest, C. E. Bibcode: 2013Natur.493..501C Altcode: It is now apparent that there are at least two heating mechanisms in the Sun's outer atmosphere, or corona. Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs 1, 2, 3). The active corona needs additional heating to reach 2,000,000-4,000,000 K this heat has been theoretically proposed to come from the reconnection and unravelling of magnetic `braids'. Evidence favouring that process has been inferred, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought to have an angular width of about 0.2 arc seconds have not been resolved. Fine-scale braiding has been seen in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating. Title: Observations from SDO, Hinode, and STEREO of a Twisting and Writhing Start to a Solar-filament-eruption Cascade Authors: Sterling, Alphonse C.; Moore, Ronald L.; Hara, Hirohisa Bibcode: 2012ApJ...761...69S Altcode: We analyze data from SDO (AIA, HMI), Hinode (SOT, XRT, EIS), and STEREO (EUVI) of a solar eruption sequence of 2011 June 1 near 16:00 UT, with an emphasis on the early evolution toward eruption. Ultimately, the sequence consisted of three emission bursts and two filament ejections. SDO/AIA 304 Å images show absorbing-material strands initially in close proximity which over ~20 minutes form a twisted structure, presumably a flux rope with ~1029 erg of free energy that triggers the resulting evolution. A jump in the filament/flux rope's displacement (average velocity ~20 km s-1) and the first burst of emission accompanies the flux-rope formation. After ~20 more minutes, the flux rope/filament kinks and writhes, followed by a semi-steady state where the flux rope/filament rises at (~5 km s-1) for ~10 minutes. Then the writhed flux rope/filament again becomes MHD unstable and violently erupts, along with rapid (50 km s-1) ejection of the filament and the second burst of emission. That ejection removed a field that had been restraining a second filament, which subsequently erupts as the second filament ejection accompanied by the third (final) burst of emission. Magnetograms from SDO/HMI and Hinode/SOT, and other data, reveal several possible causes for initiating the flux-rope-building reconnection, but we are not able to say which is dominant. Our observations are consistent with magnetic reconnection initiating the first burst and the flux-rope formation, with MHD processes initiating the further dynamics. Both filament ejections are consistent with the standard model for solar eruptions. Title: Using a global aerosol model adjoint to unravel the footprint of spatially-distributed emissions on cloud droplet number and cloud albedo Authors: Karydis, V. A.; Capps, S. L.; Moore, R. H.; Russell, A. G.; Henze, D. K.; Nenes, A. Bibcode: 2012GeoRL..3924804K Altcode: The adjoints of the GEOS-Chem Chemical Transport Model and a comprehensive cloud droplet parameterization are coupled to study the sensitivity of cloud droplet number concentration (Nd) over US regions and Central Europe to global emissions of anthropogenic fine mode aerosol precursors. Simulations reveal that the Nd over the midwestern and southeastern US is mostly sensitive to SO2 emissions during August, and to NH3 emissions during February. Over the western US, Nd is mostly sensitivity to SO2 and primary organic aerosol emissions. In Central Europe, Nd is most sensitive to NH3 and NOx emissions. As expected, local emissions strongly affect Nd; long-range transport, however, is also important for the western US and Europe. Emissions changes projected for the year 2050 are estimated to have the largest impacts on cloud albedo and Nd over Central Europe during August (42% and 82% change, respectively) and western US during February (12% and 36.5% change, respectively). Title: Dichotomy of X-Ray Jets in Solar Coronal Holes Authors: Robe, D. M.; Moore, R. L.; Falconer, D. A. Bibcode: 2012AGUFMSH51A2200R Altcode: It has been found that there are two different types of X-ray jets observed in the Sun's polar coronal holes: standard jets and blowout jets. A proposed model of this dichotomy is that a standard jet is produced by a burst of reconnection of the ambient magnetic field with the opposite-polarity leg of the base arcade. In contrast, it appears that a blowout jet is produced when the interior of the arcade has so much pent-up free magnetic energy in the form of shear and twist in the interior field that the external reconnection unleashes the interior field to erupt open. In this project, X-ray movies of the polar coronal holes taken by Hinode were searched for X-ray jets. Co-temporal movies taken by the Solar Dynamics Observatory in 304 Å emission from He II, showing solar plasma at temperatures around 80,000 K, were examined for whether the identified blowout jets carry much more He II plasma than the identified standard jets. It was found that though some jets identified as standard from the X-ray movies could be seen in the He II 304 Å movies, the blowout jets carried much more 80,000 K plasma than did most standard jets. This finding supports the proposed model for the morphology and development of the two types of jets. Title: Forecasting the Solar Drivers of Severe Space Weather from Active-Region Magnetograms Authors: Falconer, D. A.; Moore, R. L.; Barghouty, A. F.; Khazanov, I. G. Bibcode: 2012AGUFMSH51C..01F Altcode: Large flares and fast CMEs are the drivers of the most severe space weather including Solar Energetic Particle Events (SEP Events). Large flares and their co-produced CMEs are powered by the explosive release of free magnetic energy stored in non-potential magnetic fields of sunspot active regions. The free energy is stored in and released from the low-beta regime of the active region's magnetic field above the photosphere, in the chromosphere and low corona. From our work over the past decade and from similar work of several other groups, it is now well established that (1) a proxy of the free magnetic energy stored above the photosphere can be measured from photospheric magnetograms, and (2) an active region's rate of production of major CME/flare eruptions in the coming day or so is strongly correlated with its present measured value of the free-energy proxy. These results have led us to use the large database of SOHO/MDI full-disk magnetograms spanning Solar Cycle 23 to obtain empirical forecasting curves that from an active region's present measured value of the free-energy proxy give the active region's expected rates of production of major flares, CMEs, fast CMEs, and SEP Events in the coming day or so (Falconer et al 2011, Space Weather, 9, S04003). We will present these forecasting curves and demonstrate the accuracy of their forecasts. In addition, we will show that the forecasts for major flares and fast CMEs can be made significantly more accurate by taking into account not only the value of the free energy proxy but also the active region's recent productivity of major flares; specifically, whether the active region has produced a major flare (GOES class M or X) during the past 24 hours before the time of the measured magnetogram. By empirically determining the conversion of the value of free-energy proxy measured from a GONG or HMI magnetogram to that which would be measured from an MDI magnetogram, we have made GONG and HMI magnetograms useable with our MDI-based forecasting curves to forecast event rates. This work has been funded by NASA's Heliophysics Division, NSF's Division of Atmospheric Sciences, and AFOSR's MURI Program. Development of this forecasting tool for JSC/Space Radiation Analysis Group was supported by NASA's Office of Chief Engineer Technical Excellence Initiative and is supported by NASA's AES (Advance Exploration Systems) Program. Title: A Twin-CME Scenario for Ground Level Enhancement Events Authors: Li, G.; Moore, R.; Mewaldt, R. A.; Zhao, L.; Labrador, A. W. Bibcode: 2012SSRv..171..141L Altcode: 2012SSRv..tmp....1L Ground Level Enhancement (GLEs) events are extreme Solar Energetic Particle (SEP) events. Protons in these events often reach ∼GeV/nucleon. Understanding the underlying particle acceleration mechanism in these events is a major goal for Space Weather studies. In Solar Cycle 23, a total of 16 GLEs have been identified. Most of them have preceding CMEs and in-situ energetic particle observations show some of them are enhanced in ICME or flare-like material. Motivated by this observation, we discuss here a scenario in which two CMEs erupt in sequence during a short period of time from the same Active Region (AR) with a pseudo-streamer-like pre-eruption magnetic field configuration. The first CME is narrower and slower and the second CME is wider and faster. We show that the magnetic field configuration in our proposed scenario can lead to magnetic reconnection between the open and closed field lines that drape and enclose the first CME and its driven shock. The combined effect of the presence of the first shock and the existence of the open close reconnection is that when the second CME erupts and drives a second shock, one finds both an excess of seed population and an enhanced turbulence level at the front of the second shock than the case of a single CME-driven shock. Therefore, a more efficient particle acceleration will occur. The implications of our proposed scenario are discussed. Title: Prior Flaring as a Complement to Free Magnetic Energy for Forecasting Solar Eruptions Authors: Falconer, David A.; Moore, Ronald L.; Barghouty, Abdulnasser F.; Khazanov, Igor Bibcode: 2012ApJ...757...32F Altcode: From a large database of (1) 40,000 SOHO/MDI line-of-sight magnetograms covering the passage of 1300 sunspot active regions across the 30° radius central disk of the Sun, (2) a proxy of each active region's free magnetic energy measured from each of the active region's central-disk-passage magnetograms, and (3) each active region's full-disk-passage history of production of major flares and fast coronal mass ejections (CMEs), we find new statistical evidence that (1) there are aspects of an active region's magnetic field other than the free energy that are strong determinants of the active region's productivity of major flares and fast CMEs in the coming few days; (2) an active region's recent productivity of major flares, in addition to reflecting the amount of free energy in the active region, also reflects these other determinants of coming productivity of major eruptions; and (3) consequently, the knowledge of whether an active region has recently had a major flare, used in combination with the active region's free-energy proxy measured from a magnetogram, can greatly alter the forecast chance that the active region will have a major eruption in the next few days after the time of the magnetogram. The active-region magnetic conditions that, in addition to the free energy, are reflected by recent major flaring are presumably the complexity and evolution of the field. Title: Solar Spicules near and at the Limb, Observed from Hinode Authors: Sterling, A. C.; Moore, R. L. Bibcode: 2012ASPC..454...87S Altcode: Solar spicules appear as narrow jets emanating from the chromosphere and extending into the corona. They have been observed for over a hundred years, mainly in chromospheric spectral lines such as H-alpha. Because they are at the limit of visibility of ground-based instruments, their nature has long been a puzzle. In recent years however, vast progress has been made in understanding them both theoretically and observationally, as spicule studies have undergone a revolution because of the superior resolution and time cadence of ground-based and space-based instruments. Even more rapid progress is currently underway, due to the Solar Optical Telescope (SOT) instrument on the Hinode spacecraft. Here we give a synopsis of our recent findings from a movie of sharpened images from the Hinode SOT Ca II filtergraph of spicules at and near the limb in a polar coronal hole. Title: Search for a Dark Matter Candidate Produced in Association with a Single Top Quark in pp¯ Collisions at s=1.96TeV Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Anzá, F.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Fuks, B.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paulini, M.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zhou, C.; Zucchelli, S. Bibcode: 2012PhRvL.108t1802A Altcode: 2012arXiv1202.5653C We report a new search for dark matter in a data sample of an integrated luminosity of 7.7fb-1 of Tevatron pp¯ collisions at s=1.96TeV, collected by the CDF II detector. We search for production of a dark-matter candidate, D, in association with a single top quark. We consider the hadronic decay mode of the top quark exclusively, yielding a final state of three jets with missing transverse energy. The data are consistent with the standard model; we thus set 95% confidence level upper limits on the cross section of the process pp¯→t+D as a function of the mass of the dark-matter candidate. The limits are approximately 0.5 pb for a dark-matter particle with mass in the range of 0-150GeV/c2. Title: Search for Dark Matter in Events with One Jet and Missing Transverse Energy in pp¯ Collisions at s=1.96TeV Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Bai, Y.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Fox, P. J.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harnik, R.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zhou, C.; Zucchelli, S. Bibcode: 2012PhRvL.108u1804A Altcode: 2012arXiv1203.0742T We present the results of a search for dark matter production in the monojet signature. We analyze a sample of Tevatron pp¯ collisions at s=1.96TeV corresponding to an integrated luminosity of 6.7fb-1 recorded by the CDF II detector. In events with large missing transverse energy and one energetic jet, we find good agreement between the standard model prediction and the observed data. We set 90% confidence level upper limits on the dark matter production rate. The limits are translated into bounds on nucleon-dark matter scattering rates which are competitive with current direct detection bounds on spin-independent interaction below a dark matter candidate mass of 5GeV/c2, and on spin-dependent interactions up to masses of 200GeV/c2. Title: Prior Flaring: A Complement to Free Magnetic Energy for Forecasting Solar Eruptions Authors: Falconer, David; Moore, R.; Barghouty, A.; Khazanov, I. Bibcode: 2012AAS...22050803F Altcode: From a large database of (1) 40,000 SOHO/MDI line-of-sight magnetograms covering the passage of 1,300 sunspot active regions across the 30-degree radius central disk of the Sun, (2) a proxy of each active region’s free magnetic energy measured from each of the active region’s central-disk-passage magnetograms, and (3) each active region’s full-disk-passage history of production of major flares and fast coronal mass ejections (CMEs), we find new statistical evidence that (1) there are aspects of an active region’s magnetic field other than the free energy that are strong determinants of the active region’s productivity of major flares and fast CMEs in the coming few days, (2) an active region’s recent productivity of major flares, in addition to reflecting the amount of free energy in the active region, also reflects these other determinants of coming productivity of major eruptions, and (3) consequently, the knowledge of whether an active region has recently had a major flare, used in combination with the active region’s free-energy proxy measured from a magnetogram, can greatly alter the forecast chance that the active region will have a major eruption in the next few days after the time of the magnetogram. The active-region magnetic conditions that in addition to the free energy are reflected by recent major flaring are presumably the complexity of the field configuration and facets of the evolution of the field. This work has been funded by NASA’s Heliophysics Division, NSF’s Division of Atmospheric Sciences, and AFOSR’s MURI Program. Development of this forecasting tool for JSC/Space Radiation Analysis Group was supported by NASA’s Office of Chief Engineer Technical Excellence Initiative and is supported by NASA’s AES (Advance Exploration Systems) Program. Title: Search for anomalous production of multiple leptons in association with W and Z bosons at CDF Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Frisch, H.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paulini, M.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zucchelli, S. Bibcode: 2012PhRvD..85i2001A Altcode: 2012arXiv1202.1260T This paper presents a search for anomalous production of multiple low-energy leptons in association with a W or Z boson using events collected at the CDF experiment corresponding to 5.1fb-1 of integrated luminosity. This search is sensitive to a wide range of topologies with low-momentum leptons, including those with the leptons near one another. The observed rates of production of additional electrons and muons are compared with the standard model predictions. No indications of phenomena beyond the standard model are found. A 95% confidence level limit is presented on the production cross section for a benchmark model of supersymmetric hidden-valley Higgs production. Particle identification efficiencies are also provided to enable the calculation of limits on additional models. Title: The Limit of Magnetic-Shear Energy in Solar Active Regions Authors: Moore, Ronald L.; Falconer, D. A.; Sterling, A. C. Bibcode: 2012AAS...22020438M Altcode: It has been found previously, by measuring from active-region magnetograms a proxy of the free energy in the active region’s magnetic field, (1) that there is a sharp upper limit to the free energy the field can hold that increases with the amount of magnetic field in the active region, the active region’s magnetic flux content, and (2) that most active regions are near this limit when their field explodes in a CME/flare eruption. That is, explosive active regions are concentrated in a main-sequence path bordering the free-energy-limit line in (flux content, free-energy proxy) phase space. Here we present evidence that specifies the underlying magnetic condition that gives rise to the free-energy limit and the accompanying main sequence of explosive active regions. Using a suitable free energy proxy measured from vector magnetograms of 44 active regions, we find evidence that (1) in active regions at and near their free-energy limit, the ratio of magnetic-shear free energy to the non-free magnetic energy the potential field would have is of order 1 in the core field, the field rooted along the neutral line, and (2) this ratio is progressively less in active regions progressively farther below their free-energy limit. Evidently, most active regions in which this core-field energy ratio is much less than 1 cannot be triggered to explode; as this ratio approaches 1, most active regions become capable of exploding; and when this ratio is 1, most active regions are compelled to explode. This work was funded by NASA’s Science Mission Directorate through the Heliophysics Guest Investigators Program, the Hinode Project, and the Living With a Star Targeted Research & Technology Program. Title: Observations from SDO and Hinode of a Twisting and Writhing Start to a Solar-filament-eruption Cascade Authors: Sterling, Alphonse C.; Moore, R. L. Bibcode: 2012AAS...22050802S Altcode: We analyze data from SDO and hinode of a solar eruption sequence of 1 June 2011 near 16:00 UT, with emphasis on the early evolution toward eruption. Ultimately, the sequence consisted of three emission bursts and two filament ejections. SDO/AIA 304 Ang images show absorbing-material strands initially in close proximity that over 20 min form a twisted structure, presumably a flux rope with 1029 ergs of free energy that triggers the resulting evolution. A jump in the filament/flux rope's height (average velocity 20 km s-1) and the first burst of emission accompanies the flux-rope formation. After 20 min more, the flux rope/filament kinks and writhes, followed by a semi-steady state where the flux rope/filament rises at ( 5 km s-1) for 10 min. Then the writhed flux rope/filament again becomes MHD unstable and violently erupts, along with rapid (> 50 km s-1) ejection of the filament and the second burst of emission. That ejection removed field that had been restraining a second filament, which subsequently erupts as the second filament ejection accompanied by the third (final) burst of emission. Magnetograms from SDO/HMI and hinode/SOT, and other data, reveal several possible causes for initiating the flux-rope-building reconnection, but we are not able to say which is dominant. Our observations are consistent with tether-cutting reconnection initiating the first burst and the flux-rope formation, with MHD processes initiating the further dynamics. Both filament ejections are consistent with the standard model for solar eruptions. NASA supported this work through its Heliophysics program. Title: The Limit of Magnetic-shear Energy in Solar Active Regions Authors: Moore, Ronald L.; Falconer, David A.; Sterling, Alphonse C. Bibcode: 2012ApJ...750...24M Altcode: It has been found previously, by measuring from active-region magnetograms a proxy of the free energy in the active region's magnetic field, (1) that there is a sharp upper limit to the free energy the field can hold that increases with the amount of magnetic field in the active region, the active region's magnetic flux content, and (2) that most active regions are near this limit when their field explodes in a coronal mass ejection/flare eruption. That is, explosive active regions are concentrated in a main-sequence path bordering the free-energy-limit line in (flux content, free-energy proxy) phase space. Here, we present evidence that specifies the underlying magnetic condition that gives rise to the free-energy limit and the accompanying main sequence of explosive active regions. Using a suitable free-energy proxy measured from vector magnetograms of 44 active regions, we find evidence that (1) in active regions at and near their free-energy limit, the ratio of magnetic-shear free energy to the non-free magnetic energy the potential field would have is of the order of one in the core field, the field rooted along the neutral line, and (2) this ratio is progressively less in active regions progressively farther below their free-energy limit. Evidently, most active regions in which this core-field energy ratio is much less than one cannot be triggered to explode; as this ratio approaches one, most active regions become capable of exploding; and when this ratio is one, most active regions are compelled to explode. Title: Obituary: Einar A. Tandberg-Hanssen (1921-2011) Authors: Gary, G.; Emslie, A.; Hathaway, David; Moore, Ronald Bibcode: 2011BAAS...43..032G Altcode: Dr. Einar Andreas Tandberg-Hanssen was born on 6 August 1921, in Bergen, Norway, and died on July 22, 2011, in Huntsville, AL, USA, due to complications from ALS (Amyotrophic lateral sclerosis, often referred to as Lou Gehrig's disease). His parents were administrator Birger Tandberg-Hanssen (1883-1951) and secretary Antonie "Mona" Meier (1895-1967). He married Erna Rönning (27 October 1921 - 22 November 1994), a nurse, on 22 June 1951. She was the daughter of Captain Einar Rönning (1890-1969) and Borghild Lyshaug (1897-1980). Einar and Erna had two daughters, Else Biesman (and husband Allen of Rapid City, SD, USA) and Karin Brock (and husband Mike of Gulf Shores, AL, USA). At the time of his death Einar had eight grandchildren and eight great-grandchildren. Dr. Tandberg-Hanssen was an internationally-known member of the solar physics community, with over a hundred published scientific papers and several books, including Solar Activity (1967), Solar Prominences (1974), The Physics of Solar Flares (1988) and The Nature of Solar Prominences (1995). Einar grew up in Langesund and Skien, Norway, where he took the qualifying exams at Skien High School in 1941. After the war he studied natural sciences at the University of Oslo and received his undergraduate degree in astronomy in 1950. He worked as a research assistant in the Institute of Theoretical Astrophysics at the University of Oslo for three intervals in the 1950s, interspersed by fellowships at the Institut d'Astrophysique in Paris, Caltech in Pasadena, CA, the High Altitude Observatory in Boulder, CO, and the Cavendish Laboratory in the UK (at the invitation of British radio-astronomer Sir Martin Ryle). He earned a doctorate in astrophysics at the University in Oslo in 1960 with a dissertation titled "An Investigation of the Temperature Conditions in Prominences with a Special Study of the Excitation of Helium." From 1959-61, Tandberg-Hanssen was a professor at the University in Oslo. He then traveled back to the High Altitude Observatory in Boulder, Colorado, where he was employed until 1974. He was then employed at the Space Science Laboratory at NASA's Marshall Space Flight Center (MSFC) in Huntsville, Alabama. There, he was a Senior Research Scientist and later Deputy Director of the Laboratory. He served as Lab Director from 1987 until his retirement from NASA in 1993. He promptly took a part-time post within the Center for Space Plasma and Aeronomic Research at The University of Alabama in Huntsville, where he worked until his death. During his tenure at NASA, he, along with Dr. Mona Hagyard and Dr. S. T. Wu, built up a substantial, internationally-based group of solar physicists at MSFC and UA Huntsville. He was a lead investigator on two instruments aboard NASA spacecraft: the S-056 X-Ray Event Analyzer on the Skylab Apollo Telescope Mount (which provided pioneering, high-time-cadence temperature and density information on solar X-ray-emitting regions) and the Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission (which carried out sweeping new studies of EUV emission from solar active regions and flares). Dr. Tandberg-Hanssen's books about various aspects of solar activity, viz.Solar Activity (Blaisdell, 1967), Solar Prominences (Reidel, 1974), The Physics of Solar Flares (with A. G. Emslie) (Cambridge, 1988), and The Nature of Solar Prominences (Reidel, 1995), have become international standard works within the discipline of solar physics. In 1982, Dr. Tandberg-Hanssen was elected to membership in the Norwegian Academy of Science and Letters. From 1979-82 and 1982-85, respectively, he served as vice-president and president of Commission 10 of the International Astronomical Union (IAU). He served as president of the Federation of Astronomical and Geophysical Data Analysis Services from 1990-1994. He has received the NASA Exceptional Service Medal. He was also a long time editor of the journal Solar Physics. Dr. Tandberg-Hanssen's Solar Physics Memoir paper, entitled Solar Prominences - An Intriguing Phenomenon http://www.springerlink.com/content/1166j74k577kv332/ was published shortly before his death. The article starts with an autobiographical account, where the author relates how his several study-trips abroad gradually led him to the study of solar physics in general, and prominences particularly. Einar's residence as a research fellow at the Institut d'Astrophysique in Paris in the 1950s laid the foundation for a lifelong interest in France and French culture. His great interest in and knowledge of French mediaeval churches, as well as the Norwegian stave churches, is reflected in two books, Letters to My Daughters (Ivy House Pub. Group, 2004), and The Joy of Travel: More Letters to My Daughters (Pentland Press, 2007), which serve as a review, tourist guide and history book, shaped in the form of letters home to his two daughters, from his many travels in Norway and France. Einar was a true gentleman and a true scholar. As evidenced by his papers, his books, and his dealings with others, he was always seeking not only to expand his own knowledge and understanding, but also to find new ways of communicating his remarkable insight to others. He is survived by his daughters, Else and Karin, and their families. Title: Lateral Offset of the Coronal Mass Ejections from the X-flare of 2006 December 13 and Its Two Precursor Eruptions Authors: Sterling, Alphonse C.; Moore, Ronald L.; Harra, Louise K. Bibcode: 2011ApJ...743...63S Altcode: Two GOES sub-C-class precursor eruptions occurred within ~10 hr prior to and from the same active region as the 2006 December 13 X4.3-class flare. Each eruption generated a coronal mass ejection (CME) with center laterally far offset (gsim 45°) from the co-produced bright flare. Explaining such CME-to-flare lateral offsets in terms of the standard model for solar eruptions has been controversial. Using Hinode/X-Ray Telescope (XRT) and EUV Imaging Spectrometer (EIS) data, and Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO) and Michelson Doppler Imager (MDI) data, we find or infer the following. (1) The first precursor was a "magnetic-arch-blowout" event, where an initial standard-model eruption of the active region's core field blew out a lobe on one side of the active region's field. (2) The second precursor began similarly, but the core-field eruption stalled in the side-lobe field, with the side-lobe field erupting ~1 hr later to make the CME either by finally being blown out or by destabilizing and undergoing a standard-model eruption. (3) The third eruption, the X-flare event, blew out side lobes on both sides of the active region and clearly displayed characteristics of the standard model. (4) The two precursors were offset due in part to the CME originating from a side-lobe coronal arcade that was offset from the active region's core. The main eruption (and to some extent probably the precursor eruptions) was offset primarily because it pushed against the field of the large sunspot as it escaped outward. (5) All three CMEs were plausibly produced by a suitable version of the standard model. Title: Observed Aspects of Reconnection in Solar Eruptions Authors: Moore, Ronald L.; Sterling, Alphonse C.; Gary, G. Allen; Cirtain, Jonathan W.; Falconer, David A. Bibcode: 2011SSRv..160...73M Altcode: 2011SSRv..tmp..113M; 2011SSRv..tmp..189M; 2011SSRv..tmp...30M The observed magnetic field configuration and signatures of reconnection in the large solar magnetic eruptions that make major flares and coronal mass ejections and in the much smaller magnetic eruptions that make X-ray jets are illustrated with cartoons and representative observed eruptions. The main reconnection signatures considered are the imaged bright emission from the heated plasma on reconnected field lines. In any of these eruptions, large or small, the magnetic field that drives the eruption and/or that drives the buildup to the eruption is initially a closed bipolar arcade. From the form and configuration of the magnetic field in and around the driving arcade and from the development of the reconnection signatures in coordination with the eruption, we infer that (1) at the onset of reconnection the reconnection current sheet is small compared to the driving arcade, and (2) the current sheet can grow to the size of the driving arcade only after reconnection starts and the unleashed erupting field dynamically forces the current sheet to grow much larger, building it up faster than the reconnection can tear it down. We conjecture that the fundamental reason the quasi-static pre-eruption field is prohibited from having a large current sheet is that the magnetic pressure is much greater than the plasma pressure in the chromosphere and low corona in eruptive solar magnetic fields. Title: Confirmation of the 'Main Sequence' of Explosive Active Regions Authors: Falconer, David Allen; Moore, Ron Bibcode: 2011shin.confE..45F Altcode: We study the dependence of production of major CME/flare eruptions on the source active region's (AR's) location in (flux content, free energy) phase space. For this, an AR's flux content and a proxy of its free magnetic energy content can be adequately measured from 96-minute cadence SOHO/MDI magnetograms when the AR is within 30 degrees of disk center (Falconer et al 2008, ApJ, 688, 143). The AR's evolution in this phase space can thereby be tracked as it crosses the central disk. By our definition, an AR is (1) mature if its flux is growing by less than 50%/day when it rotates onto the 30-degree-radius central disk, or (2) emerging if its flux is growing faster than 50%/day when it enters the central disk or if it is born within the central disk. In an initial study of 46 ARs, 44 were mature and 2 were emerging. From 1800 MDI magnetograms of mature ARs, we found that (1) mature ARs have a sharp upper bound on the free energy they can attain that increases with increasing flux content, and (2) for mature ARs, nearly all CMEs and X-class flares are produced by ARs that are near the free-energy limit line. These ARs constitute the main sequence of explosive mature ARs (Falconer et al 2009, ApJ, 700, L166). The two emerging ARs attained free energy well beyond the limit for mature ARs of the same flux content, questioning whether emerging ARs have a free-energy limit and explosive main sequence like those for mature ARs. Here, from a much larger sample, we (1) confirm the free-energy limit and explosive main sequence for mature ARs, and (2) show that emerging ARs do have a free-energy limit and an explosive main sequence, each offset to higher free energy relative to its mature-AR counterpart. This work was funded by NSF SHINE Program and by the AFOSR MURI Program. Title: The Main Sequence of Explosive Emerging Solar Active Regions Authors: Falconer, David; Moore, R. Bibcode: 2011SPD....42.2304F Altcode: 2011BAAS..43S.2304F We study the dependence of production of major CME/flare eruptions on the source active region's (AR's) location in (flux content, free energy) phase space. For this, an AR's flux content and a proxy of its free magnetic energy content can be adequately measured from 96-minute cadence SOHO/MDI magnetograms when the AR is within 30 degrees of disk center (Falconer et al 2008, ApJ, 688, 143). The AR's evolution in this phase space can thereby be tracked as it crosses the central disk. By our definition, an AR is (1) mature if its flux is growing by less than 50%/day when it rotates onto the 30-degree-radius central disk, or (2) emerging if its flux is growing faster than 50%/day when it enters the central disk or if it is born within the central disk. In an initial study of 46 ARs, 42 were mature and 4 were emerging. From 1800 MDI magnetograms of the 42 mature ARs, we found that (1) mature ARs have a sharp upper bound on the free energy they can attain that increases with increasing flux content, and (2) for mature ARs, nearly all CMEs and X-class flares are produced by ARs that are near the free-energy limit line. These ARs constitute the main sequence of explosive mature ARs (Falconer et al 2009, ApJ, 700, L166). Two of the four emerging ARs attained free energy well beyond the limit for mature ARs of the same flux content, questioning whether emerging ARs have a free-energy limit and explosive main sequence like those for mature ARs. Here, we show from a much larger sample of ARs ( 1000), of which about 1/3 are emerging, that emerging ARs do have a free-energy limit and a explosive main sequence, each offset to higher free energy relative to its mature-AR counterpart. Title: The Reason for the Main Sequence of Explosive Solar Active Regions Authors: Moore, Ronald L.; Falconer, D. A. Bibcode: 2011SPD....42.2305M Altcode: 2011BAAS..43S.2305M From measurement of magnetic flux and a proxy of free magnetic energy from 1800 SOHO/MDI line-of-sight magnetograms of 44 sunspot active regions, Falconer et al (2009, ApJ, 700, L169) showed (1) there is an upper limit to the free magnetic energy an active region can hold, (2) this limit increases with active-region magnetic size (flux content), (3) most major CME/flare eruptions are produce by active regions that are near their free-energy limit, (4) in (flux content, free-energy proxy) phase space, the source active regions for major CME/flare eruptions are concentrated along a main sequence, a path that runs close below the free-energy limit line, and (5) the free-energy limit and the main sequence probably result from the steep increase in CME/flare productivity as an active region approaches its free-energy limit, depleting the active region's free energy as fast as it is built up. Here we present (1) a new direct proxy of an active region's free magnetic energy, and (2) a corresponding proxy of the ratio of free energy to potential-field energy in the more-nonpotential parts of the active region. Each is measured from a vector magnetogram of the active region. From these two magnetic-energy proxies measured from Marshall Space Flight Center vector magnetograms of 42 of the active regions of Falconer et al (2009), we (1) affirm that the free-energy proxy measured in Falconer et al (2009) is indeed a proxy of an active region's free magnetic energy, (2) further support the above reason for the main sequence of explosive active regions, and (3) conclude that magnetic fields in active regions become ready to explode and produce CME/flare eruptions when their free energy becomes comparable to the potiential-field energy. This work was supported by funding from NASA's Heliophysics Division, NSF's Division of Atmospheric Sciences, and AFOSR's MURI Program. Title: Insights into Filament Eruption Onset from Solar Dynamics Observatory Observations Authors: Sterling, Alphonse C.; Moore, R. L.; Freeland, S. L. Bibcode: 2011SPD....42.0904S Altcode: 2011BAAS..43S.0904S We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging 3 km/s, with a step-like trajectory. Accompanying a final rise step 20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds 50 km/s prior to the preflare brightening and appear more helical, with speeds 50-100 km/s, after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell "cocoon" of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start 5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting. A full description of this work appears in ApJ Letters 2011, 731, L3. NASA supported this work through its Solar Physics Supporting Research and Technology, Sun-Earth Connection Guest Investigator, and Living With a Star Targeted Research & Technology programs. Title: A tool for empirical forecasting of major flares, coronal mass ejections, and solar particle events from a proxy of active-region free magnetic energy Authors: Falconer, David; Barghouty, Abdulnasser F.; Khazanov, Igor; Moore, Ron Bibcode: 2011SpWea...9.4003F Altcode: This paper describes a new forecasting tool developed for and currently being tested by NASA's Space Radiation Analysis Group (SRAG) at Johnson Space Center, which is responsible for the monitoring and forecasting of radiation exposure levels of astronauts. The new software tool is designed for the empirical forecasting of M- and X-class flares, coronal mass ejections, and solar energetic particle events. For each type of event, the algorithm is based on the empirical relationship between the event rate and a proxy of the active region's free magnetic energy. Each empirical relationship is determined from a data set of ∼40,000 active-region magnetograms from ∼1300 active regions observed by SOHO/Michelson Doppler Imager (MDI) that have known histories of flare, coronal mass ejection, and solar energetic particle event production. The new tool automatically extracts each strong-field magnetic area from an MDI full-disk magnetogram, identifies each as a NOAA active region, and measures the proxy of the active region's free magnetic energy from the extracted magnetogram. For each active region, the empirical relationship is then used to convert the free-magnetic-energy proxy into an expected event rate. The expected event rate in turn can be readily converted into the probability that the active region will produce such an event in a given forward time window. Descriptions of the data sets, algorithm, and software in addition to sample applications and a validation test are presented. Further development and transition of the new tool in anticipation of SDO/HMI are briefly discussed. Title: Insights into Filament Eruption Onset from Solar Dynamics Observatory Observations Authors: Sterling, Alphonse C.; Moore, Ronald L.; Freeland, Samuel L. Bibcode: 2011ApJ...731L...3S Altcode: We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging ~3 km s-1, with a step-like trajectory. Accompanying a final rise step ~20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds ~50 km s-1 prior to the preflare brightening and appear more helical, with speeds ~50-100 km s-1, after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell "cocoon" of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start ~5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting. Title: Solar X-ray Jets, Type-II Spicules, Granule-size Emerging Bipoles, and the Genesis of the Heliosphere Authors: Moore, Ronald L.; Sterling, Alphonse C.; Cirtain, Jonathan W.; Falconer, David A. Bibcode: 2011ApJ...731L..18M Altcode: From Hinode observations of solar X-ray jets, Type-II spicules, and granule-size emerging bipolar magnetic fields in quiet regions and coronal holes, we advocate a scenario for powering coronal heating and the solar wind. In this scenario, Type-II spicules and Alfvén waves are generated by the granule-size emerging bipoles (EBs) in the manner of the generation of X-ray jets by larger magnetic bipoles. From observations and this scenario, we estimate that Type-II spicules and their co-generated Alfvén waves carry into the corona an area-average flux of mechanical energy of ~7 × 105 erg cm-2 s-1. This is enough to power the corona and solar wind in quiet regions and coronal holes, and therefore indicates that the granule-size EBs are the main engines that generate and sustain the entire heliosphere. Title: Refractories, Structure and Properties of Authors: Moore, R. E. Bibcode: 2011emst.book.8079M Altcode: The definition of "refractory" employed as an adjective is variously applied; to people, it means obstinate or unmanageable, and to things such as ores, it means hard to reduce or to fuse. This latter usage is correct for refractory ceramic materials, which possess the key characteristic of refractoriness, i.e., they are difficult to fuse. Refractory ceramics are inorganic chemical substances, single or polyphase in nature, which are processed at high temperature and/or are intended for high-temperature applications. They are employed wherever a process involves treatment or exposure at elevated temperatures, e.g., the smelting of metals, the sintering of ceramics, the melting of glass, the processing of hydrocarbons and other chemicals, etc. Title: First results for the Solar Ultraviolet Magnetograph Investigation (SUMI) Authors: Moore, R. L.; Cirtain, J. W.; West, E.; Kobayashi, K.; Robinson, B.; Winebarger, A. R.; Tarbell, T. D.; de Pontieu, B.; McIntosh, S. W. Bibcode: 2010AGUFMSH11B1655M Altcode: On July 31, 2010 SUMI was launched to 286km above the White Sands Missile Range to observe active region 11092. SUMI is a spectro-polarimeter capable of measuring the spectrum for Mg II h & k at 280 nm and C IV at 155 nm. Simultaneous observations with Hinode and SDO provide total coverage of the region from the photosphere into the corona, a very unique and original data set. We will present the initial results from this first flight of the experiment and demonstrate the utility of further observations by SUMI. Title: 24-Hour Forecasting of CME/Flare Eruptions from Active-Region Magnetograms (Invited) Authors: Falconer, D. A.; Barghouty, A.; Khazanov, I. G.; Moore, R. L. Bibcode: 2010AGUFMSH54D..04F Altcode: We have developed an automated tool for forecasting severe space weather from full-disk magnetograms. This tool is now being used on a trial basis by NASA’s Space Radiation Analysis Group (SRAG) at JSC. SRAG is responsible for the monitoring and forecasting of exposure the astronauts to particle radiation. The tool is described in Falconer, Barghouty, Khazanov, and Moore (2010), submitted to Space Weather. The new software tool is designed for the empirical forecasting of M- and X-class flares, coronal mass ejections, and solar energetic particle events. For each of these event types, the algorithm is based on the empirical relationship between the event rate and a proxy of the active region’s free magnetic energy. The relationship is determined from ~40,000 active-region magnetograms from ~1,300 active regions that were observed within 30 heliographic degrees from disk center by SOHO/MDI, and that have known histories of flare, coronal mass ejection, and solar energetic particle event production during disk passage. The tool automatically extracts each strong-field magnetic areas from an MDI full-disk magnetogram, identifies each as a NOAA active region, and measures the proxy of the active region’s free magnetic energy from the extracted magnetogram. For each active region, the empirical relationship is then used to convert the free magnetic energy proxy into the active region’s expected event rate (see figure). The expected event rate in turn can be readily converted into the probability that the active region will produce such an event in a given forward time window. We can make this tool applicable to the full-disk line-of-sight magnetograms from SDO/HMI or as a backup, from NSO/GONG. By empirically determining the conversion of the value of free-energy proxy measured from an HMI magnetogram to that which would be measured from an MDI magnetogram, we can use the HMI magnetograms with the empirical relationships determined from our MDI data base to make forecasts of event rates. This work was funded by the NASA Technical Excellence Initiative, by the AFOSR MURI Program, and by the NASA LWS TR&T Program. Title: On the Origin of the Solar Moreton Wave of 2006 December 6 Authors: Balasubramaniam, K. S.; Cliver, E. W.; Pevtsov, A.; Temmer, M.; Henry, T. W.; Hudson, H. S.; Imada, S.; Ling, A. G.; Moore, R. L.; Muhr, N.; Neidig, D. F.; Petrie, G. J. D.; Veronig, A. M.; Vršnak, B.; White, S. M. Bibcode: 2010ApJ...723..587B Altcode: We analyzed ground- and space-based observations of the eruptive flare (3B/X6.5) and associated Moreton wave (~850 km s-1 ~270° azimuthal span) of 2006 December 6 to determine the wave driver—either flare pressure pulse (blast) or coronal mass ejection (CME). Kinematic analysis favors a CME driver of the wave, despite key gaps in coronal data. The CME scenario has a less constrained/smoother velocity versus time profile than is the case for the flare hypothesis and requires an acceleration rate more in accord with observations. The CME picture is based, in part, on the assumption that a strong and impulsive magnetic field change observed by a GONG magnetograph during the rapid rise phase of the flare corresponds to the main acceleration phase of the CME. The Moreton wave evolution tracks the inferred eruption of an extended coronal arcade, overlying a region of weak magnetic field to the west of the principal flare in NOAA active region 10930. Observations of Hα foot point brightenings, disturbance contours in off-band Hα images, and He I 10830 Å flare ribbons trace the eruption from 18:42 to 18:44 UT as it progressed southwest along the arcade. Hinode EIS observations show strong blueshifts at foot points of this arcade during the post-eruption phase, indicating mass outflow. At 18:45 UT, the Moreton wave exhibited two separate arcs (one off each flank of the tip of the arcade) that merged and coalesced by 18:47 UT to form a single smooth wave front, having its maximum amplitude in the southwest direction. We suggest that the erupting arcade (i.e., CME) expanded laterally to drive a coronal shock responsible for the Moreton wave. We attribute a darkening in Hα from a region underlying the arcade to absorption by faint unresolved post-eruption loops. Title: Fibrillar Chromospheric Spicule-like Counterparts to an Extreme-ultraviolet and Soft X-ray Blowout Coronal Jet Authors: Sterling, Alphonse C.; Harra, Louise K.; Moore, Ronald L. Bibcode: 2010ApJ...722.1644S Altcode: We observe an erupting jet feature in a solar polar coronal hole, using data from Hinode/Solar Optical Telescope (SOT), Extreme Ultraviolet Imaging Spectrometer (EIS), and X-Ray Telescope (XRT), with supplemental data from STEREO/EUVI. From extreme-ultraviolet (EUV) and soft X-ray (SXR) images we identify the erupting feature as a blowout coronal jet: in SXRs it is a jet with a bright base, and in EUV it appears as an eruption of relatively cool (~50,000 K) material of horizontal size scale ~30'' originating from the base of the SXR jet. In SOT Ca II H images, the most pronounced analog is a pair of thin (~1'') ejections at the locations of either of the two legs of the erupting EUV jet. These Ca II features eventually rise beyond 45'', leaving the SOT field of view, and have an appearance similar to standard spicules except that they are much taller. They have velocities similar to that of "type II" spicules, ~100 km s-1, and they appear to have spicule-like substructures splitting off from them with horizontal velocity ~50 km s-1, similar to the velocities of splitting spicules measured by Sterling et al. Motions of splitting features and of other substructures suggest that the macroscopic EUV jet is spinning or unwinding as it is ejected. This and earlier work suggest that a subpopulation of Ca II type II spicules are the Ca II manifestation of portions of larger scale erupting magnetic jets. A different subpopulation of type II spicules could be blowout jets occurring on a much smaller horizontal size scale than the event we observe here. Title: Evidence for magnetic flux cancelation leading to an ejective solar eruption observed by Hinode, TRACE, STEREO, and SoHO/MDI Authors: Sterling, A. C.; Chifor, C.; Mason, H. E.; Moore, R. L.; Young, P. R. Bibcode: 2010A&A...521A..49S Altcode: