Author name code: kopp-greg ADS astronomy entries on 2022-09-14 author:"Kopp, Greg A." ------------------------------------------------------------------------ Title: Variability of the Sun's Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone Authors: Vieira, L. E. A.; Kopp, G.; Dudok de Wit, T.; da Silva, L. A.; Carlesso, F.; Barbosa, A. R.; Muralikrishna, A.; Santos, R. Bibcode: 2022ApJS..260...38V Altcode: 2022arXiv220402940V Luminosity, which is the total amount of radiant energy emitted by an object, is one of the most critical quantities in astrophysics for characterizing stars. Equally important is the temporal evolution of a star's luminosity because of its intimate connection with the stellar energy budget, large-scale convective motion, and heat storage in the stellar interior. The Sun's luminosity and its variation have not been measured to date because current observations of the solar radiative output have been restricted to vantage points near the Earth. Here, we model the solar luminosity by extending a semiempirical total solar irradiance (TSI) model that uses solar-surface magnetism to reconstruct solar irradiance over the entire 4π solid angle around the Sun. This model was constrained by comparing its output to the irradiance in the Earth's direction with the measured TSI. Comparing the solar luminosity to the TSI on timescales from days to solar cycles for cycles 23 and 24, we find poor agreement on short timescales (<solar rotation). This is not unexpected due to the Earth-centric viewing geometry and short-term irradiance dependence on surface features on the Earth-facing solar disk. On longer timescales, however, we find good agreement between the luminosity model and the TSI, which suggests that the extrapolation of luminosities to multicycle timescales based on TSI reconstructions may be possible. We show that the solar luminosity is not constant but varies in phase with the solar cycle. This variation has an amplitude of 0.14% from minimum to maximum for Solar Cycle 23. Considering the energetics in the solar convection zone, it is therefore obvious that a steady-state input from the radiative zone at the solar minimum level would lead to a gradual reduction in the energy content in the convection zone over multicentury timescales. We show that the luminosity at the base of the convection zone should be approximately 0.032% higher than that at the solar surface during solar minimum to maintain net energy equilibrium through the solar cycle. These different energy-input scenarios place constraints on the long-term evolution of the TSI and its impact on the solar forcing of climate variability. These results highlight the convection zone's role as an energy reservoir on solar-cycle timescales and set constraints for dynamo models intending to understand the long-term evolution of the Sun and solar analogs. Title: Solar-Cycle Variability Results from the Solar Radiation and Climate Experiment (SORCE) Mission Authors: Woods, Thomas N.; Harder, Jerald W.; Kopp, Greg; Snow, Martin Bibcode: 2022SoPh..297...43W Altcode: The Solar Radiation and Climate Experiment (SORCE) was a NASA mission that operated from 2003 to 2020 to provide key climate-monitoring measurements of total solar irradiance (TSI) and solar spectral irradiance (SSI). This 17-year mission made TSI and SSI observations during the declining phase of Solar Cycle 23, during all of Solar Cycle 24, and at the very beginning of Solar Cycle 25. The SORCE solar-variability results include comparisons of the solar irradiance observed during Solar Cycles 23 and 24 and the solar-cycle minima levels in 2008 - 2009 and 2019 - 2020. The differences between these two minima are very small and are not significantly above the estimate of instrument stability over the 11-year period. There are differences in the SSI variability for Solar Cycles 23 and 24, notably for wavelengths longer than 250 nm. Consistency comparisons with SORCE variability on solar-rotation timescales and solar-irradiance model predictions suggest that the SORCE Solar Cycle 24 SSI results might be more accurate than the SORCE Solar Cycle 23 results. The SORCE solar-variability results have been useful for many Sun-climate studies and will continue to serve as a reference for comparisons with future missions studying solar variability. Title: Final Report for SAG 21: The Effect of Stellar Contamination on Space-based Transmission Spectroscopy Authors: Rackham, Benjamin V.; Espinoza, Néstor; Berdyugina, Svetlana V.; Korhonen, Heidi; MacDonald, Ryan J.; Montet, Benjamin T.; Morris, Brett M.; Oshagh, Mahmoudreza; Shapiro, Alexander I.; Unruh, Yvonne C.; Quintana, Elisa V.; Zellem, Robert T.; Apai, Dániel; Barclay, Thomas; Barstow, Joanna K.; Bruno, Giovanni; Carone, Ludmila; Casewell, Sarah L.; Cegla, Heather M.; Criscuoli, Serena; Fischer, Catherine; Fournier, Damien; Giampapa, Mark S.; Giles, Helen; Iyer, Aishwarya; Kopp, Greg; Kostogryz, Nadiia M.; Krivova, Natalie; Mallonn, Matthias; McGruder, Chima; Molaverdikhani, Karan; Newton, Elisabeth R.; Panja, Mayukh; Peacock, Sarah; Reardon, Kevin; Roettenbacher, Rachael M.; Scandariato, Gaetano; Solanki, Sami; Stassun, Keivan G.; Steiner, Oskar; Stevenson, Kevin B.; Tregloan-Reed, Jeremy; Valio, Adriana; Wedemeyer, Sven; Welbanks, Luis; Yu, Jie; Alam, Munazza K.; Davenport, James R. A.; Deming, Drake; Dong, Chuanfei; Ducrot, Elsa; Fisher, Chloe; Gilbert, Emily; Kostov, Veselin; López-Morales, Mercedes; Line, Mike; Močnik, Teo; Mullally, Susan; Paudel, Rishi R.; Ribas, Ignasi; Valenti, Jeff A. Bibcode: 2022arXiv220109905R Altcode: Study Analysis Group 21 (SAG21) of the Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, and plages. This SAG has brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies"). Title: Four, Three, Two, One... Whats Up (or Down) with the TSI Instruments? Authors: Kopp, Greg; Coddington, Odele; Dudok de Wit, Thierry; Harber, David; Heuerman, Karl; Lean, Judith; Upton, Lisa; Wang, Yi-Ming Bibcode: 2021AGUFMGC24E..04K Altcode: Over the last three years, the number of spaceborne instruments producing measurements of the total solar irradiance (TSI), the TOA net incoming energy powering the Earths climate system, has decreased from four to one. This 43-year-long record of solar variability has depended on continuity and overlap of successive instruments but is now completely reliant on the Total Irradiance Monitor flying on the International Space Station. Fortunately, this is a short-term trend in this climate data record and not an intended long-term trend. We summarize the recent turnover (or, more correctly, turn-off) causing the declining number in the instrument suite contributing to the TSI record. Then, before extrapolating-based panic might set in, we provide a more optimistic look at the future of these measurements and the several instruments currently being readied for launch, some of which include fresh designs enabled by new materials and calibration approaches. We will also discuss updates to a composite TSI record using the entire collection of instruments from the spacecraft era as well as mentioning the accuracies and stabilities of the recent measurements. Finally, we mention an effort underway to extend the TSI record to historical times via updates to sunspot-number records, modern flux-transport models, and proxy-based TSI-reconstruction models. Title: Reconstructing solar irradiance from historical Ca II K observations. I. Method and its validation Authors: Chatzistergos, Theodosios; Krivova, Natalie A.; Ermolli, Ilaria; Yeo, Kok Leng; Mandal, Sudip; Solanki, Sami K.; Kopp, Greg; Malherbe, Jean-Marie Bibcode: 2021A&A...656A.104C Altcode: 2021arXiv210905844C Context. Knowledge of solar irradiance variability is critical to Earth's climate models and understanding the solar influence on Earth's climate. Direct solar irradiance measurements have only been available since 1978. Reconstructions of past variability typically rely on sunspot data. However, sunspot records provide only indirect information on the facular and network regions, which are decisive contributors to irradiance variability on timescales of the solar cycle and longer.
Aims: Our ultimate goal is to reconstruct past solar irradiance variations using historical full-disc Ca II K observations to describe the facular contribution independently of sunspot observations. Here, we develop the method and test it extensively by using modern CCD-based (charge-coupled device) Ca II K observations. We also carry out initial tests on two photographic archives.
Methods: We employ carefully reduced and calibrated Ca II K images from 13 datasets, including some of the most prominent series, such as those from the Meudon, Mt Wilson, and Rome observatories. We convert them to unsigned magnetic field maps and then use them as input to the adapted Spectral and Total Irradiance Reconstruction (SATIRE) model to reconstruct total solar irradiance (TSI) variations over the period 1978-2019, for which direct irradiance measurements are available.
Results: The reconstructed irradiance from the analysed Ca II K archives agrees well with direct irradiance measurements and existing reconstructions. The model also returns good results on data taken with different bandpasses and images with low spatial resolution. Historical Ca II K archives suffer from numerous inconsistencies, but we show that these archives can still be used to reconstruct TSI with reasonable accuracy provided the observations are accurately processed and the effects of changes in instrumentation and instrumental parameters are identified and accounted for. The reconstructions are relatively insensitive to the TSI reference record used to fix the single free parameter of the model. Furthermore, even employment of a series, itself reconstructed from Ca II K data, as a reference for further reconstructions returns nearly equally accurate results. This will enable the Ca II K archives without an overlap with direct irradiance measurements to be used to reconstruct past irradiance.
Conclusions: By using the unsigned magnetic maps of the Sun reconstructed from modern high-quality Ca II K observations as input into the SATIRE model, we can reconstruct solar irradiance variations nearly as accurately as from directly recorded magnetograms. Historical Ca II K observations can also be used for past irradiance reconstructions but need additional care, for example identifying and accounting for discontinuities and changes in the quality of the data with time. Title: Science Highlights and Final Updates from 17 Years of Total Solar Irradiance Measurements from the SOlar Radiation and Climate Experiment/Total Irradiance Monitor (SORCE/TIM) Authors: Kopp, Greg Bibcode: 2021SoPh..296..133K Altcode: The final version (V.19) of the total solar irradiance data from the SOlar Radiation and Climate Experiment (SORCE) Total Irradiance Monitor has been released. This version includes all calibrations updated to the end of the mission and provides irradiance data from 25 February 2003 through 25 February 2020. These final calibrations are presented along with the resulting final data products. An overview of the on-orbit operations timeline is provided as well as the associated changes in the time-dependent uncertainties. Scientific highlights from the instrument are also presented. These include the establishment of a new, lower TSI value; accuracy improvements to other TSI instruments via a new calibration facility; the lowest on-orbit noise (for high sensitivity to solar variability) of any TSI instrument; the best inherent stability of any on-orbit TSI instrument; a lengthy (17-year) measurement record benefitting from these stable, low-noise measurements; the first reported detection of a solar flare in TSI; and observations of two Venus transits and four Mercury transits. Title: Overview of the Solar Radiation and Climate Experiment (SORCE) Seventeen-Year Mission Authors: Woods, Thomas N.; Harder, Jerald W.; Kopp, Greg; McCabe, Debra; Rottman, Gary; Ryan, Sean; Snow, Martin Bibcode: 2021SoPh..296..127W Altcode: The Solar Radiation and Climate Experiment (SORCE) was a NASA mission that operated from 2003 to 2020 to provide key climate-monitoring measurements of total solar irradiance (TSI) and solar spectral irradiance (SSI). Three important accomplishments of the SORCE mission are i) the continuation of the 42-year-long TSI climate data record, ii) the continuation of the ultraviolet SSI record, and iii) the initiation of the near-ultraviolet, visible, and near-infrared SSI records. All of the SORCE instruments functioned well over the 17-year mission, which far exceeded its five-year prime mission goal. The SORCE spacecraft, having mostly redundant subsystems, was also robust over the mission. The end of the SORCE mission was a planned passivation of the spacecraft following a successful two-year overlap with the NASA Total and Spectral Solar Irradiance Sensor (TSIS) mission, which continues the TSI and SSI climate records. There were a couple of instrument anomalies and a few spacecraft anomalies during SORCE's long mission, but operational changes and updates to flight software enabled SORCE to remain productive to the end of its mission. The most challenging of the anomalies was the degradation of the battery capacity that began to impact operations in 2009 and was the cause for the largest SORCE data gap (August 2013 - February 2014). An overview of the SORCE mission is provided with a couple of science highlights and a discussion of flight anomalies that impacted the solar observations. Companion articles about the SORCE instruments and their final science data-processing algorithms provide additional details about the instrument measurements over the duration of the mission. Title: Measuring and modeling the variability of solar Balmer lines Authors: Criscuoli, S.; Marchenko, S.; Deland, M.; Choudhary, D.; Kopp, G. Bibcode: 2021AAS...23811312C Altcode: We investigate the variability of solar Balmer lines (H-alpha, beta, gamma, delta) observed by space-borne radiometers (SORCE, SCIAMACHY, GOME-2, OMI, and TROPOMI), combining these precise, long-term observations with abundant, high-resolution data from the ground-based NSO/ISS spectrograph. We relate the detected variability to the appearance of magnetic features on the solar disk. We find that on solar-rotation timescales Balmer line activity indices (defined as line-core to line-wing ratios) closely follow variations in the total solar irradiance (which is predominantly photospheric), thus frequently (specifically, during passages of big sunspot groups) deviates from behavior of the line-activity indices that track chromospheric activity levels. At longer timescales (years), the correlation with chromospheric indices increases, with periods of low- or even anti- correlation found at intermediate timescales. Comparisons with Balmer-line variability patterns obtained from a semi-empirical model indicate that it is unlikely that the periods of low/anti correlations can be ascribed to the presence of filaments, in contradiction to some previous studies. Title: Historical TSI Reconstructions: Calibrating the Polar Fields in the Advective Flux Transport Model Using Joy's Law Tilt Authors: Upton, L.; Coddington, O.; Kopp, G.; Lean, J. Bibcode: 2021AAS...23830407U Altcode: Historical reconstructions of total solar irradiance (TSI) rely on estimates of the solar open and closed magnetic flux obtained by simulating the flux emergence and transport. The Advective Flux Transport (AFT) model is a realistic surface flux transport model that has demonstrated its ability to reproduce flux emergence and evolution on the Sun. We have created synthetic active region databases based on the Sunspot Indices and Long-term Solar Observations (SILSO) 2.0 revised sunspot-number record. These synthetic databases include the timing, position, Joy's tilt, and strength of solar active regions and have been used as input into AFT to create historical reconstructions. While these reconstructions produce realistic magnetic maps and solar cycles with alternating Hale's polarity, the change in the polar axial dipole (which is the basis for the estimates of the open flux) from the beginning of the cycle to the end of the cycle was weaker than expected. We show that modifying the distribution of Joy's Law tilt (i.e., the scatter about the standard Joy's Law tilt) allows us to modulate the rate at which the polar fields change. In particular, we find that increasing the variability in Joy's Law tilt significantly increases the change in the polar axial dipole from one cycle to the next. We have used the observed relationship between the strength of the polar fields at minimum and the amplitude of the next solar cycle to estimate how much the axial dipolar fields should change over the course of each historical cycle. We then modify the Joy's Law tilt distribution in each cycle to ensure that desired change in the polar fields for that cycle is achieved. In this way, we are able to calibrate the polar field evolution in the simulations to produce more realistic solar cycles. Finally, we show the impact that these changes have on the historical reconstructions of TSI. Title: Irradiance Variations of the Sun and Sun-Like Stars - Overview of Topical Collection Authors: Kopp, Greg; Shapiro, Alexander Bibcode: 2021SoPh..296...60K Altcode: 2021arXiv210206913K This topical collection summarizes recent advances in observing and modeling irradiance variations of the Sun and Sun-like stars, emphasizing the links between surface magnetic fields and the resulting solar and stellar variability. In particular, the articles composing this collection summarize recent progress in i) solar-irradiance measurements; ii) modeling of solar- and stellar-irradiance variability; and iii) understanding of the effects of such variability on Earth's climate and exoplanet environments. This topical-collection overview article gives background and more details on these aspects of variability. Title: Understanding variability of solar Balmer lines Authors: Criscuoli, Serena; Marchenko, Sergey; DeLand, Matthew; Choudary, Debi; Kopp, Greg Bibcode: 2021csss.confE.290C Altcode: Precise, adequately high-cadence, long-term records of spectral variability at different temporal scales lead to better understanding of a wide variety of phenomena including stellar atmospheres and dynamos, evolution of the magnetic fields on a stellar photosphere, convective motions, and rotational periods. These, in turn, are fundamental for the detectability of exoplanets, the characterization of their atmospheres and habitability, as well as characterization of stellar magnetospheres and winds. The Sun, viewed as a star via spectral irradiance measurements, offers a means of exploring such measurements while also having the imaging capability to help discern the causes of observed spectral variations. In this study, we investigate the variability of solar Balmer lines (H-α, β, γ and δ) observed by space-borne radiometers, combining these precise, long-term observations with abundant, high-resolution data from the ground-based NSO/ISS spectrograph. We relate the detected variability to magnetic features on the solar disk. We find that on solar-rotation timescales (~month), the Balmer line activity indices (defined as line-core to line-wing ratios) closely follow variations in the total solar irradiance (which is predominantly photospheric), thus frequently (specifically, during passages of big sunspot groups) deviates from behavior of the line-activity indices that track chromospheric activity levels. At longer timescales (years), the correlation with chromospheric indices increases, with periods of low- or even anti- correlation found at intermediate timescales. Comparisons with Balmer-line variability patterns obtained from a semi-empirical model indicate the periods of low/anti correlations should be attributed to the increase of the relative abundance of network, which affects the Ca-index while leaving almost un-altered the Hα-index. Title: Solar activity and responses observed in Balmer lines Authors: Marchenko, S.; Criscuoli, S.; DeLand, M. T.; Choudhary, D. P.; Kopp, G. Bibcode: 2021A&A...646A..81M Altcode: Context. Many stars show Sun-like magnetic activity cycles, which are frequently observed by tracking changes in the chromospherically sensitive CaII H&K doublet. However, relationships between the line profile changes related to the magnetic activity seen in strong spectral transitions in other portions of a stellar spectrum are yet to be understood.
Aims: We follow variability patterns in various solar lines in order to relate them to the emergence, passage, and decay of active solar regions.
Methods: The line activity indices (core-to-wing ratio) for the upper Balmer lines - Hβ, Hγ, and Hδ - are constructed from the near-daily solar measurements acquired by the Ozone Monitoring Instrument and the TROPOspheric Monitoring Instrument.
Results: On solar rotation timescales, the upper Balmer line activity indices closely follow variations in the total solar irradiance, r ∼ -(0.6 - 0.7), and thus frequently deviate from the behavior of the line activity indices that track chromospheric activity levels (e.g., the CH 430 nm band used in this study), specifically during passages of big sunspot groups. Title: Historical Solar Irradiance Using the Updated Sunspot Record Authors: Kopp, G.; Coddington, O.; Lean, J.; Upton, L. Bibcode: 2020AGUFMA227.0006K Altcode: The total solar irradiance (TSI), which is by far the largest contributor to the energy input to the Earth's climate system, has been measured from space for the last four decades. Earth-climate studies rely on long-duration records, for which this is only beginning to qualify. To extend this record back in time and enable lengthier correlations with other Earth-climate data records, solar-irradiance models are used. One such is the NRLTSI model, which uses TSI measurement-era correlations with solar proxies to estimate historical TSI values via the temporal extensions enabled by those proxies. The longest-duration direct-measurement solar proxy is the sunspot record, which spans over 400 years now. Reevaluations of that record via reanalyzes of the original data records, the discovery of new sunspot records, and different combinations of observers' records via new analytical methods have led to the Solar Index and Long-term Solar Observations (SILSO) V.2 sunspot record. This new record, shown in red in the figure, shows much higher sunspot counts and different temporal variability than the prior (V.1) record (shown in green in the figure). Title: Changing of the Guard for Total Solar Irradiance Authors: Kopp, G. Bibcode: 2020AGUFMA237...05K Altcode: The Total Irradiance Monitor (TIM) on the SORCE mission established an accuracy of total solar irradiance (TSI) measurements that was about ten times better than previous instruments achieved. The instrument also demonstrated improvements in inherent stability, being four to twenty times better than other spacecraft instruments. Both of these achievements are due to an improved design over prior such instruments. The SORCE/TIM continued on to achieve several other notable accomplishments, including the first detection of a solar flare in TSI, measuring the largest short-term solar-irradiance decrease recorded during the spacecraft era, and observing six planetary transits. Its primary accomplishment, however, may be contributing one of the longest-duration time series of the TSI to the critical solar-climate data record, being 17 years (and one day) long (shown in red in the figure).

The fourth successor to this innovative and stalwart instrument has now been built and launched. The TSIS-1/TIM began regular measurements in early 2018, providing two years of overlap with the SORCE/TIM before the latter was decommissioned in Feb. 2020. The TSIS-1/TIM has improved accuracies over those of even the SORCE/TIM, and is currently the only TSI instrument providing publicly-available data to maintain the 42-year-long spaceborne TSI measurement record. Title: 1/f noise in irradiance records affects our understanding of trends in solar radiative forcing Authors: Dudok de Wit, T.; Kopp, G. Bibcode: 2020AGUFMA237...08D Altcode: One of the critical issues in solar irradiance observations is the making of records that are long enough to 1) have sufficient overlap between different missions to determine instrument offsets and 2) to distinguish actual solar trends from instrumental effects. Different approaches have been developed for quantifying the minimal duration of such records or for determing when a perceived trend is real.

Recently, we have found that the noise of total solar irradiance radiometers tends to follow a 1/f scaling, which is also known as flicker noise. 1/f noise stands out by having long-range correlations and properties that are substantially different from the usual (and often implicitly assumed) white noise. Here we show how this 1/f noise deeply impacts our perception of trends in irradiance observations, whose assessment requires much greater care. Title: NASA's Solar Radiation and Climate Experiment (SORCE) Final Data Products of Solar Irradiance from 2003 to 2020 Authors: Sandoval, L.; Merkel, A. W.; Beland, S.; Penton, S. V.; Stone, B.; Elliott, J. P.; Harder, J. W.; Snow, M. A.; Kopp, G.; McClintock, W. E.; Woods, T. N. Bibcode: 2020AGUFMA227.0010S Altcode: The Spectral Irradiance Monitor (SIM), the SOlar Stellar Irradiance Comparison Experiment (SOLSTICE), the XUV Photometer System (XPS), and the Total Irradiance Monitor (TIM) instruments on the Solar Radiation and Climate Experiment (SORCE) spacecraft took daily solar spectral irradiance (SSI) and total solar irradiance (TSI) measurements since April and February 2003, respectively. The SORCE was decommissioned on February 25, 2020 at which time the SORCE mission began its final mission phase (Phase-F). All final data products and documents, as well as all selected ancillary information, have been organized in compliance with NASA's Earth Science Data Preservation Content Specification (423-SPEC-001), archived at the NASA Goddard Earth Sciences Data and Information Services Center (GES DISC), and made available to the public. We describe the data, documentation, and the various formats that have been selected for archival. Title: Evidence for Top Quark Production in Nucleus-Nucleus Collisions Authors: Sirunyan, A. M.; Tumasyan, A.; Adam, W.; Ambrogi, F.; Bergauer, T.; Dragicevic, M.; Erö, J.; Escalante Del Valle, A.; Frühwirth, R.; Jeitler, M.; Krammer, N.; Lechner, L.; Liko, D.; Madlener, T.; Mikulec, I.; Rad, N.; Schieck, J.; Schöfbeck, R.; Spanring, M.; Templ, S.; Waltenberger, W.; Wulz, C. -E.; Zarucki, M.; Chekhovsky, V.; Litomin, A.; Makarenko, V.; Suarez Gonzalez, J.; Darwish, M. R.; De Wolf, E. A.; Di Croce, D.; Janssen, X.; Kello, T.; Lelek, A.; Pieters, M.; Rejeb Sfar, H.; Van Haevermaet, H.; Van Mechelen, P.; Van Putte, S.; Van Remortel, N.; Blekman, F.; Bols, E. S.; Chhibra, S. S.; D'Hondt, J.; De Clercq, J.; Lontkovskyi, D.; Lowette, S.; Marchesini, I.; Moortgat, S.; Python, Q.; Tavernier, S.; Van Doninck, W.; Van Mulders, P.; Beghin, D.; Bilin, B.; Clerbaux, B.; De Lentdecker, G.; Delannoy, H.; Dorney, B.; Favart, L.; Grebenyuk, A.; Kalsi, A. K.; Makarenko, I.; Moureaux, L.; Pétré, L.; Popov, A.; Postiau, N.; Starling, E.; Thomas, L.; Vander Velde, C.; Vanlaer, P.; Vannerom, D.; Wezenbeek, L.; Cornelis, T.; Dobur, D.; Khvastunov, I.; Niedziela, M.; Roskas, C.; Skovpen, K.; Tytgat, M.; Verbeke, W.; Vermassen, B.; Vit, M.; Bruno, G.; Bury, F.; Caputo, C.; David, P.; Delaere, C.; Delcourt, M.; Donertas, I. S.; Giammanco, A.; Lemaitre, V.; Prisciandaro, J.; Saggio, A.; Taliercio, A.; Teklishyn, M.; Vischia, P.; Wuyckens, S.; Zobec, J.; Alves, G. A.; Correia Silva, G.; Hensel, C.; Moraes, A.; Aldá Júnior, W. L.; Belchior Batista Das Chagas, E.; Carvalho, W.; Chinellato, J.; Coelho, E.; Da Costa, E. M.; Da Silveira, G. G.; De Jesus Damiao, D.; Fonseca De Souza, S.; Malbouisson, H.; Martins, J.; Matos Figueiredo, D.; Medina Jaime, M.; Melo De Almeida, M.; Mora Herrera, C.; Mundim, L.; Nogima, H.; Rebello Teles, P.; Sanchez Rosas, L. J.; Santoro, A.; Silva Do Amaral, S. M.; Sznajder, A.; Thiel, M.; Tonelli Manganote, E. J.; Torres Da Silva De Araujo, F.; Vilela Pereira, A.; Bernardes, C. A.; Calligaris, L.; Fernandez Perez Tomei, T. R.; Gregores, E. M.; Lemos, D. S.; Mercadante, P. G.; Novaes, S. F.; Padula, Sandra S.; Aleksandrov, A.; Antchev, G.; Atanasov, I.; Hadjiiska, R.; Iaydjiev, P.; Misheva, M.; Rodozov, M.; Shopova, M.; Sultanov, G.; Bonchev, M.; Dimitrov, A.; Ivanov, T.; Litov, L.; Pavlov, B.; Petkov, P.; Petrov, A.; Fang, W.; Guo, Q.; Wang, H.; Yuan, L.; Ahmad, M.; Hu, Z.; Wang, Y.; Chapon, E.; Chen, G. M.; Chen, H. S.; Chen, M.; Jiang, C. H.; Leggat, D.; Liao, H.; Liu, Z.; Sharma, R.; Spiezia, A.; Tao, J.; Wang, J.; Zhang, H.; Zhang, S.; Zhao, J.; Agapitos, A.; Ban, Y.; Chen, C.; Chen, G.; Levin, A.; Li, J.; Li, L.; Li, Q.; Lyu, X.; Mao, Y.; Qian, S. J.; Wang, D.; Wang, Q.; Xiao, J.; You, Z.; Gao, X.; Xiao, M.; Avila, C.; Cabrera, A.; Florez, C.; Fraga, J.; Sarkar, A.; Segura Delgado, M. A.; Mejia Guisao, J.; Ramirez, F.; Ruiz Alvarez, J. D.; Salazar González, C. A.; Vanegas Arbelaez, N.; Giljanovic, D.; Godinovic, N.; Lelas, D.; Puljak, I.; Sculac, T.; Antunovic, Z.; Kovac, M.; Brigljevic, V.; Ferencek, D.; Majumder, D.; Mesic, B.; Roguljic, M.; Starodumov, A.; Susa, T.; Ather, M. W.; Attikis, A.; Erodotou, E.; Ioannou, A.; Kole, G.; Kolosova, M.; Konstantinou, S.; Mavromanolakis, G.; Mousa, J.; Nicolaou, C.; Ptochos, F.; Razis, P. A.; Rykaczewski, H.; Saka, H.; Tsiakkouri, D.; Finger, M.; Finger, M.; Kveton, A.; Tomsa, J.; Ayala, E.; Carrera Jarrin, E.; Salama, E.; Lotfy, A.; Mahmoud, M. A.; Bhowmik, S.; Carvalho Antunes De Oliveira, A.; Dewanjee, R. K.; Ehataht, K.; Kadastik, M.; Raidal, M.; Veelken, C.; Eerola, P.; Forthomme, L.; Kirschenmann, H.; Osterberg, K.; Voutilainen, M.; Brücken, E.; Garcia, F.; Havukainen, J.; Karimäki, V.; Kim, M. S.; Kinnunen, R.; Lampén, T.; Lassila-Perini, K.; Laurila, S.; Lehti, S.; Lindén, T.; Siikonen, H.; Tuominen, E.; Tuominiemi, J.; Luukka, P.; Tuuva, T.; Besancon, M.; Couderc, F.; Dejardin, M.; Denegri, D.; Faure, J. L.; Ferri, F.; Ganjour, S.; Givernaud, A.; Gras, P.; Hamel de Monchenault, G.; Jarry, P.; Leloup, C.; Lenzi, B.; Locci, E.; Malcles, J.; Rander, J.; Rosowsky, A.; Sahin, M. Ö.; Savoy-Navarro, A.; Titov, M.; Yu, G. B.; Ahuja, S.; Amendola, C.; Beaudette, F.; Bonanomi, M.; Busson, P.; Charlot, C.; Davignon, O.; Diab, B.; Falmagne, G.; Granier de Cassagnac, R.; Kucher, I.; Lobanov, A.; Martin Perez, C.; Nguyen, M.; Ochando, C.; Paganini, P.; Rembser, J.; Salerno, R.; Sauvan, J. B.; Sirois, Y.; Zabi, A.; Zghiche, A.; Agram, J. -L.; Andrea, J.; Bloch, D.; Bourgatte, G.; Brom, J. -M.; Chabert, E. 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H.; Barney, D.; Bendavid, J.; Bianco, M.; Bocci, A.; Bortignon, P.; Bossini, E.; Brondolin, E.; Camporesi, T.; Cerminara, G.; Cristella, L.; d'Enterria, D.; Dabrowski, A.; Daci, N.; Daponte, V.; David, A.; De Roeck, A.; Deile, M.; Di Maria, R.; Dobson, M.; Dünser, M.; Dupont, N.; Elliott-Peisert, A.; Emriskova, N.; Fallavollita, F.; Fasanella, D.; Fiorendi, S.; Franzoni, G.; Fulcher, J.; Funk, W.; Giani, S.; Gigi, D.; Gill, K.; Glege, F.; Gouskos, L.; Gruchala, M.; Guilbaud, M.; Gulhan, D.; Hegeman, J.; Iiyama, Y.; Innocente, V.; James, T.; Janot, P.; Kaspar, J.; Kieseler, J.; Komm, M.; Kratochwil, N.; Lange, C.; Lecoq, P.; Long, K.; Lourenço, C.; Malgeri, L.; Mannelli, M.; Massironi, A.; Meijers, F.; Mersi, S.; Meschi, E.; Moortgat, F.; Mulders, M.; Ngadiuba, J.; Niedziela, J.; Orfanelli, S.; Orsini, L.; Pantaleo, F.; Pape, L.; Perez, E.; Peruzzi, M.; Petrilli, A.; Petrucciani, G.; Pfeiffer, A.; Pierini, M.; Pitters, F. M.; Rabady, D.; Racz, A.; Rieger, M.; Rovere, M.; Sakulin, H.; Salfeld-Nebgen, J.; Scarfi, S.; Schäfer, C.; Schwick, C.; Selvaggi, M.; Sharma, A.; Silva, P.; Snoeys, W.; Sphicas, P.; Steggemann, J.; Summers, S.; Tavolaro, V. R.; Treille, D.; Tsirou, A.; Van Onsem, G. P.; Vartak, A.; Verzetti, M.; Wozniak, K. A.; Zeuner, W. D.; Caminada, L.; Erdmann, W.; Horisberger, R.; Ingram, Q.; Kaestli, H. C.; Kotlinski, D.; Langenegger, U.; Rohe, T.; Backhaus, M.; Berger, P.; Calandri, A.; Chernyavskaya, N.; Dissertori, G.; Dittmar, M.; Donegà, M.; Dorfer, C.; Gadek, T.; Gómez Espinosa, T. A.; Grab, C.; Hits, D.; Lustermann, W.; Lyon, A. -M.; Manzoni, R. A.; Meinhard, M. T.; Micheli, F.; Musella, P.; Nessi-Tedaldi, F.; Pauss, F.; Perovic, V.; Perrin, G.; Perrozzi, L.; Pigazzini, S.; Ratti, M. G.; Reichmann, M.; Reissel, C.; Reitenspiess, T.; Ristic, B.; Ruini, D.; Sanz Becerra, D. A.; Schönenberger, M.; Shchutska, L.; Stampf, V.; Vesterbacka Olsson, M. L.; Wallny, R.; Zhu, D. H.; Amsler, C.; Botta, C.; Brzhechko, D.; Canelli, M. F.; De Cosa, A.; Del Burgo, R.; Heikkilä, J. K.; Huwiler, M.; Jofrehei, A.; Kilminster, B.; Leontsinis, S.; Macchiolo, A.; Mikuni, V. M.; Molinatti, U.; Neutelings, I.; Rauco, G.; Robmann, P.; Schweiger, K.; Takahashi, Y.; Wertz, S.; Adloff, C.; Kuo, C. M.; Lin, W.; Roy, A.; Sarkar, T.; Yu, S. S.; Ceard, L.; Chang, P.; Chao, Y.; Chen, K. F.; Chen, P. H.; Hou, W. -S.; Li, Y. y.; Lu, R. -S.; Paganis, E.; Psallidas, A.; Steen, A.; Yazgan, E.; Asavapibhop, B.; Asawatangtrakuldee, C.; Srimanobhas, N.; Boran, F.; Damarseckin, S.; Demiroglu, Z. S.; Dolek, F.; Dozen, C.; Dumanoglu, I.; Eskut, E.; Gokbulut, G.; Guler, Y.; Gurpinar Guler, E.; Hos, I.; Isik, C.; Kangal, E. E.; Kara, O.; Kayis Topaksu, A.; Kiminsu, U.; Onengut, G.; Ozdemir, K.; Polatoz, A.; Simsek, A. E.; Tali, B.; Tok, U. G.; Turkcapar, S.; Zorbakir, I. S.; Zorbilmez, C.; Isildak, B.; Karapinar, G.; Ocalan, K.; Yalvac, M.; Atakisi, I. O.; Gülmez, E.; Kaya, M.; Kaya, O.; Özçelik, Ö.; Tekten, S.; Yetkin, E. A.; Cakir, A.; Cankocak, K.; Komurcu, Y.; Sen, S.; Aydogmus Sen, F.; Cerci, S.; Kaynak, B.; Ozkorucuklu, S.; Sunar Cerci, D.; Grynyov, B.; Levchuk, L.; Bhal, E.; Bologna, S.; Brooke, J. J.; Burns, D.; Clement, E.; Cussans, D.; Flacher, H.; Goldstein, J.; Heath, G. P.; Heath, H. F.; Kreczko, L.; Krikler, B.; Paramesvaran, S.; Sakuma, T.; Seif El Nasr-Storey, S.; Smith, V. J.; Taylor, J.; Titterton, A.; Bell, K. W.; Belyaev, A.; Brew, C.; Brown, R. M.; Cockerill, D. J. A.; Ellis, K. V.; Harder, K.; Harper, S.; Linacre, J.; Manolopoulos, K.; Newbold, D. M.; Olaiya, E.; Petyt, D.; Reis, T.; Schuh, T.; Shepherd-Themistocleous, C. H.; Thea, A.; Tomalin, I. R.; Williams, T.; Bainbridge, R.; Bloch, P.; Bonomally, S.; Borg, J.; Breeze, S.; Buchmuller, O.; Bundock, A.; Cepaitis, V.; Chahal, G. S.; Colling, D.; Dauncey, P.; Davies, G.; Della Negra, M.; Everaerts, P.; Fedi, G.; Hall, G.; Iles, G.; Langford, J.; Lyons, L.; Magnan, A. -M.; Malik, S.; Martelli, A.; Milosevic, V.; Morton, A.; Nash, J.; Palladino, V.; Pesaresi, M.; Raymond, D. M.; Richards, A.; Rose, A.; Scott, E.; Seez, C.; Shtipliyski, A.; Stoye, M.; Tapper, A.; Uchida, K.; Virdee, T.; Wardle, N.; Webb, S. N.; Winterbottom, D.; Zecchinelli, A. G.; Zenz, S. C.; Cole, J. E.; Hobson, P. R.; Khan, A.; Kyberd, P.; Mackay, C. K.; Reid, I. D.; Teodorescu, L.; Zahid, S.; Brinkerhoff, A.; Call, K.; Caraway, B.; Dittmann, J.; Hatakeyama, K.; Madrid, C.; McMaster, B.; Pastika, N.; Smith, C.; Bartek, R.; Dominguez, A.; Uniyal, R.; Vargas Hernandez, A. M.; Buccilli, A.; Charaf, O.; Cooper, S. I.; Gleyzer, S. V.; Henderson, C.; Rumerio, P.; West, C.; Akpinar, A.; Albert, A.; Arcaro, D.; Cosby, C.; Demiragli, Z.; Gastler, D.; Richardson, C.; Rohlf, J.; Salyer, K.; Sperka, D.; Spitzbart, D.; Suarez, I.; Yuan, S.; Zou, D.; Benelli, G.; Burkle, B.; Coubez, X.; Cutts, D.; Duh, Y. t.; Hadley, M.; Heintz, U.; Hogan, J. M.; Kwok, K. H. M.; Laird, E.; Landsberg, G.; Lau, K. T.; Lee, J.; Narain, M.; Sagir, S.; Syarif, R.; Usai, E.; Wong, W. Y.; Yu, D.; Zhang, W.; Band, R.; Brainerd, C.; Breedon, R.; Calderon De La Barca Sanchez, M.; Chertok, M.; Conway, J.; Conway, R.; Cox, P. T.; Erbacher, R.; Flores, C.; Funk, G.; Jensen, F.; Ko, W.; Kukral, O.; Lander, R.; Mulhearn, M.; Pellett, D.; Pilot, J.; Shi, M.; Taylor, D.; Tos, K.; Tripathi, M.; Yao, Y.; Zhang, F.; Bachtis, M.; Bravo, C.; Cousins, R.; Dasgupta, A.; Florent, A.; Hamilton, D.; Hauser, J.; Ignatenko, M.; Lam, T.; Mccoll, N.; Nash, W. A.; Regnard, S.; Saltzberg, D.; Schnaible, C.; Stone, B.; Valuev, V.; Burt, K.; Chen, Y.; Clare, R.; Gary, J. W.; Ghiasi Shirazi, S. M. A.; Hanson, G.; Karapostoli, G.; Long, O. R.; Manganelli, N.; Olmedo Negrete, M.; Paneva, M. I.; Si, W.; Wimpenny, S.; Zhang, Y.; Branson, J. G.; Chang, P.; Cittolin, S.; Cooperstein, S.; Deelen, N.; Derdzinski, M.; Duarte, J.; Gerosa, R.; Gilbert, D.; Hashemi, B.; Klein, D.; Krutelyov, V.; Letts, J.; Masciovecchio, M.; May, S.; Padhi, S.; Pieri, M.; Sharma, V.; Tadel, M.; Würthwein, F.; Yagil, A.; Amin, N.; Bhandari, R.; Campagnari, C.; Citron, M.; Dorsett, A.; Dutta, V.; Incandela, J.; Marsh, B.; Mei, H.; Ovcharova, A.; Qu, H.; Quinnan, M.; Richman, J.; Sarica, U.; Stuart, D.; Wang, S.; Anderson, D.; Bornheim, A.; Cerri, O.; Dutta, I.; Lawhorn, J. M.; Lu, N.; Mao, J.; Newman, H. B.; Nguyen, T. Q.; Pata, J.; Spiropulu, M.; Vlimant, J. R.; Xie, S.; Zhang, Z.; Zhu, R. Y.; Alison, J.; Andrews, M. B.; Ferguson, T.; Mudholkar, T.; Paulini, M.; Sun, M.; Vorobiev, I.; Weinberg, M.; Cumalat, J. P.; Ford, W. T.; MacDonald, E.; Mulholland, T.; Patel, R.; Perloff, A.; Stenson, K.; Ulmer, K. A.; Wagner, S. R.; Alexander, J.; Cheng, Y.; Chu, J.; Cranshaw, D. J.; Datta, A.; Frankenthal, A.; Mcdermott, K.; Monroy, J.; Patterson, J. R.; Quach, D.; Ryd, A.; Sun, W.; Tan, S. M.; Tao, Z.; Thom, J.; Wittich, P.; Zientek, M.; Abdullin, S.; Albrow, M.; Alyari, M.; Apollinari, G.; Apresyan, A.; Apyan, A.; Banerjee, S.; Bauerdick, L. A. T.; Beretvas, A.; Berry, D.; Berryhill, J.; Bhat, P. C.; Burkett, K.; Butler, J. N.; Canepa, A.; Cerati, G. B.; Cheung, H. W. K.; Chlebana, F.; Cremonesi, M.; Elvira, V. D.; Freeman, J.; Gecse, Z.; Gottschalk, E.; Gray, L.; Green, D.; Grünendahl, S.; Gutsche, O.; Harris, R. M.; Hasegawa, S.; Heller, R.; Herwig, T. C.; Hirschauer, J.; Jayatilaka, B.; Jindariani, S.; Johnson, M.; Joshi, U.; Klijnsma, T.; Klima, B.; Kortelainen, M. J.; Lammel, S.; Lewis, J.; Lincoln, D.; Lipton, R.; Liu, M.; Liu, T.; Lykken, J.; Maeshima, K.; Mason, D.; McBride, P.; Merkel, P.; Mrenna, S.; Nahn, S.; O'Dell, V.; Papadimitriou, V.; Pedro, K.; Pena, C.; Prokofyev, O.; Ravera, F.; Reinsvold Hall, A.; Ristori, L.; Schneider, B.; Sexton-Kennedy, E.; Smith, N.; Soha, A.; Spalding, W. J.; Spiegel, L.; Stoynev, S.; Strait, J.; Taylor, L.; Tkaczyk, S.; Tran, N. V.; Uplegger, L.; Vaandering, E. W.; Wang, M.; Weber, H. A.; Woodard, A.; Acosta, D.; Avery, P.; Bourilkov, D.; Cadamuro, L.; Cherepanov, V.; Errico, F.; Field, R. D.; Guerrero, D.; Joshi, B. M.; Kim, M.; Konigsberg, J.; Korytov, A.; Lo, K. H.; Matchev, K.; Menendez, N.; Mitselmakher, G.; Rosenzweig, D.; Shi, K.; Wang, J.; Wang, S.; Zuo, X.; Joshi, Y. R.; Adams, T.; Askew, A.; Diaz, D.; Habibullah, R.; Hagopian, S.; Hagopian, V.; Johnson, K. F.; Khurana, R.; Kolberg, T.; Martinez, G.; Prosper, H.; Schiber, C.; Yohay, R.; Zhang, J.; Baarmand, M. M.; Butalla, S.; Elkafrawy, T.; Hohlmann, M.; Noonan, D.; Rahmani, M.; Saunders, M.; Yumiceva, F.; Adams, M. R.; Apanasevich, L.; Becerril Gonzalez, H.; Cavanaugh, R.; Chen, X.; Dittmer, S.; Evdokimov, O.; Gerber, C. E.; Hangal, D. A.; Hofman, D. J.; Mills, C.; Oh, G.; Roy, T.; Tonjes, M. B.; Varelas, N.; Viinikainen, J.; Wang, H.; Wang, X.; Wu, Z.; Alhusseini, M.; Bilki, B.; Dilsiz, K.; Durgut, S.; Gandrajula, R. P.; Haytmyradov, M.; Khristenko, V.; Köseyan, O. K.; Merlo, J. -P.; Mestvirishvili, A.; Moeller, A.; Nachtman, J.; Ogul, H.; Onel, Y.; Ozok, F.; Penzo, A.; Snyder, C.; Tiras, E.; Wetzel, J.; Yi, K.; Amram, O.; Blumenfeld, B.; Corcodilos, L.; Eminizer, M.; Gritsan, A. V.; Kyriacou, S.; Maksimovic, P.; Mantilla, C.; Roskes, J.; Swartz, M.; Vámi, T. Á.; Baldenegro Barrera, C.; Baringer, P.; Bean, A.; Bylinkin, A.; Isidori, T.; Khalil, S.; King, J.; Krintiras, G.; Kropivnitskaya, A.; Lindsey, C.; Mcbrayer, W.; Minafra, N.; Murray, M.; Rogan, C.; Royon, C.; Sanders, S.; Schmitz, E.; Tapia Takaki, J. D.; Wang, Q.; Williams, J.; Wilson, G.; Duric, S.; Ivanov, A.; Kaadze, K.; Kim, D.; Maravin, Y.; Mendis, D. R.; Mitchell, T.; Modak, A.; Mohammadi, A.; Rebassoo, F.; Wright, D.; Adams, E.; Baden, A.; Baron, O.; Belloni, A.; Eno, S. C.; Feng, Y.; Hadley, N. J.; Jabeen, S.; Jeng, G. Y.; Kellogg, R. G.; Koeth, T.; Mignerey, A. C.; Nabili, S.; Seidel, M.; Skuja, A.; Tonwar, S. C.; Wang, L.; Wong, K.; Abercrombie, D.; Allen, B.; Bi, R.; Brandt, S.; Busza, W.; Cali, I. A.; Chen, Y.; D'Alfonso, M.; Gomez Ceballos, G.; Goncharov, M.; Harris, P.; Hsu, D.; Hu, M.; Klute, M.; Kovalskyi, D.; Krupa, J.; Lee, Y. -J.; Luckey, P. D.; Maier, B.; Marini, A. C.; Mcginn, C.; Mironov, C.; Narayanan, S.; Niu, X.; Paus, C.; Rankin, D.; Roland, C.; Roland, G.; Shi, Z.; Stephans, G. S. F.; Sumorok, K.; Tatar, K.; Velicanu, D.; Wang, J.; Wang, T. W.; Wang, Z.; Wyslouch, B.; Chatterjee, R. M.; Evans, A.; Guts, S.; Hansen, P.; Hiltbrand, J.; Jain, Sh.; Krohn, M.; Kubota, Y.; Lesko, Z.; Mans, J.; Revering, M.; Rusack, R.; Saradhy, R.; Schroeder, N.; Strobbe, N.; Wadud, M. A.; Acosta, J. G.; Oliveros, S.; Bloom, K.; Chauhan, S.; Claes, D. R.; Fangmeier, C.; Finco, L.; Golf, F.; González Fernández, J. R.; Kravchenko, I.; Siado, J. E.; Snow, G. R.; Stieger, B.; Tabb, W.; Agarwal, G.; Harrington, C.; Iashvili, I.; Kharchilava, A.; McLean, C.; Nguyen, D.; Parker, A.; Pekkanen, J.; Rappoccio, S.; Roozbahani, B.; Alverson, G.; Barberis, E.; Freer, C.; Haddad, Y.; Hortiangtham, A.; Madigan, G.; Marzocchi, B.; Morse, D. M.; Nguyen, V.; Orimoto, T.; Skinnari, L.; Tishelman-Charny, A.; Wamorkar, T.; Wang, B.; Wisecarver, A.; Wood, D.; Bhattacharya, S.; Bueghly, J.; Chen, Z.; Gilbert, A.; Gunter, T.; Hahn, K. A.; Odell, N.; Schmitt, M. H.; Sung, K.; Velasco, M.; Bucci, R.; Dev, N.; Goldouzian, R.; Hildreth, M.; Hurtado Anampa, K.; Jessop, C.; Karmgard, D. J.; Lannon, K.; Li, W.; Loukas, N.; Marinelli, N.; Mcalister, I.; Meng, F.; Mohrman, K.; Musienko, Y.; Ruchti, R.; Siddireddy, P.; Taroni, S.; Wayne, M.; Wightman, A.; Wolf, M.; Zygala, L.; Alimena, J.; Bylsma, B.; Cardwell, B.; Durkin, L. S.; Francis, B.; Hill, C.; Ji, W.; Lefeld, A.; Winer, B. L.; Yates, B. R.; Dezoort, G.; Elmer, P.; Greenberg, B.; Haubrich, N.; Higginbotham, S.; Kalogeropoulos, A.; Kopp, G.; Kwan, S.; Lange, D.; Lucchini, M. T.; Luo, J.; Marlow, D.; Mei, K.; Ojalvo, I.; Olsen, J.; Palmer, C.; Piroué, P.; Stickland, D.; Tully, C.; Malik, S.; Norberg, S.; Barnes, V. E.; Chawla, R.; Das, S.; Gutay, L.; Jones, M.; Jung, A. W.; Mahakud, B.; Negro, G.; Neumeister, N.; Peng, C. C.; Piperov, S.; Qiu, H.; Schulte, J. F.; Trevisani, N.; Wang, F.; Xiao, R.; Xie, W.; Cheng, T.; Dolen, J.; Parashar, N.; Baty, A.; Dildick, S.; Ecklund, K. M.; Freed, S.; Geurts, F. J. M.; Kilpatrick, M.; Kumar, A.; Li, W.; Padley, B. P.; Redjimi, R.; Roberts, J.; Rorie, J.; Shi, W.; Stahl Leiton, A. G.; Tu, Z.; Zhang, A.; Bodek, A.; de Barbaro, P.; Demina, R.; Dulemba, J. L.; Fallon, C.; Ferbel, T.; Galanti, M.; Garcia-Bellido, A.; Hindrichs, O.; Khukhunaishvili, A.; Ranken, E.; Taus, R.; Chiarito, B.; Chou, J. P.; Gandrakota, A.; Gershtein, Y.; Halkiadakis, E.; Hart, A.; Heindl, M.; Hughes, E.; Kaplan, S.; Karacheban, O.; Laflotte, I.; Lath, A.; Montalvo, R.; Nash, K.; Osherson, M.; Salur, S.; Schnetzer, S.; Somalwar, S.; Stone, R.; Thayil, S. A.; Thomas, S.; Acharya, H.; Delannoy, A. G.; Spanier, S.; Bouhali, O.; Dalchenko, M.; Delgado, A.; Eusebi, R.; Gilmore, J.; Huang, T.; Kamon, T.; Kim, H.; Luo, S.; Malhotra, S.; Marley, D.; Mueller, R.; Overton, D.; Perniè, L.; Rathjens, D.; Safonov, A.; Akchurin, N.; Damgov, J.; Hegde, V.; Kunori, S.; Lamichhane, K.; Lee, S. W.; Mengke, T.; Muthumuni, S.; Peltola, T.; Undleeb, S.; Volobouev, I.; Wang, Z.; Whitbeck, A.; Appelt, E.; Greene, S.; Gurrola, A.; Janjam, R.; Johns, W.; Maguire, C.; Melo, A.; Ni, H.; Padeken, K.; Romeo, F.; Sheldon, P.; Tuo, S.; Velkovska, J.; Verweij, M.; Ang, L.; Arenton, M. W.; Cox, B.; Cummings, G.; Hakala, J.; Hirosky, R.; Joyce, M.; Ledovskoy, A.; Neu, C.; Tannenwald, B.; Wang, Y.; Wolfe, E.; Xia, F.; Karchin, P. E.; Poudyal, N.; Sturdy, J.; Thapa, P.; Black, K.; Bose, T.; Buchanan, J.; Caillol, C.; Dasu, S.; De Bruyn, I.; Dodd, L.; Galloni, C.; He, H.; Herndon, M.; Hervé, A.; Hussain, U.; Lanaro, A.; Loeliger, A.; Loveless, R.; Madhusudanan Sreekala, J.; Mallampalli, A.; Pinna, D.; Ruggles, T.; Savin, A.; Shang, V.; Sharma, V.; Smith, W. H.; Teague, D.; Trembath-reichert, S.; Vetens, W.; CMS Collaboration Bibcode: 2020PhRvL.125v2001S Altcode: Ultrarelativistic heavy ion collisions recreate in the laboratory the thermodynamical conditions prevailing in the early universe up to 10-6 sec , thereby allowing the study of the quark-gluon plasma (QGP), a state of quantum chromodynamics (QCD) matter with deconfined partons. The top quark, the heaviest elementary particle known, is accessible in nucleus-nucleus collisions at the CERN LHC, and constitutes a novel probe of the QGP. Here, we report the first evidence for the production of top quarks in nucleus-nucleus collisions, using lead-lead collision data at a nucleon-nucleon center-of-mass energy of 5.02 TeV recorded by the CMS experiment. Two methods are used to measure the cross section for top quark pair production (σt t ¯ ) via the selection of charged leptons (electrons or muons) and bottom quarks. One method relies on the leptonic information alone, and the second one exploits, in addition, the presence of bottom quarks. The measured cross sections, σt t ¯=2.5 4-0.74+0.84 and 2.03-0.64+0.71 μ b , respectively, are compatible with expectations from scaled proton-proton data and QCD predictions. Title: VizieR Online Data Catalog: Faculae-Spot dominance & rotation periods (Amazo-Gomez+, 2020) Authors: Amazo-Gomez, E. M.; Shapiro, A. I.; Solanki, S. K.; Kopp, G.; Oshagh, M.; Reinhold, T.; Reiners, A. Bibcode: 2020yCat..36420225A Altcode: This table contains an example of the GPS outputs, the compared rotation period values from GLS and ACF, and stellar parameters for Kepler stars.

In column 4 and 5 values of alpha-factor and its 2-sigma uncertainty are reported respectively. Prot GPS values in column 6, as result of applying Eq. 1 using the factor alpha=0.19. 2) Column 7 shows the Prot reported by Reinhold & Gizon (2015, Cat. J/A+A/583/A65). 3) Prot and variability values reported by McQuillan et al. (2014, Cat. J/ApJS/211/24) in column 8. 4) Columns 10, 11 and 12 show the logg, [Fe/H], and Teff respectively, taken from Huber et al. (2014, Cat J/ApJS/211/2).

(1 data file). Title: Inflection point in the power spectrum of stellar brightness variations. III. Facular versus spot dominance on stars with known rotation periods Authors: Amazo-Gómez, E. M.; Shapiro, A. I.; Solanki, S. K.; Kopp, G.; Oshagh, M.; Reinhold, T.; Reiners, A. Bibcode: 2020A&A...642A.225A Altcode: 2020arXiv200811492A Context. Stellar rotation periods can be determined by observing brightness variations caused by active magnetic regions transiting visible stellar disk as the star rotates. Successful stellar photometric surveys stemming from the Kepler and TESS observations have led to the determination of rotation periods in tens of thousands of young and active stars. However, there is still a lack of information on the rotation periods of older and less active stars like the Sun. The irregular temporal profiles of light curves caused by the decay times of active regions, which are comparable to, or even shorter than, stellar rotation periods, in combination with the random emergence of active regions make period determination for such stars very difficult.
Aims: We tested the performance of a new method for the determination of stellar rotation periods against stars with previously determined rotation periods. The method is based on calculating the gradient of the power spectrum (GPS) and identifying the position of the inflection point (i.e. point with the highest gradient). The GPS method is specifically aimed at determining rotation periods of low-activity stars like the Sun.
Methods: We applied the GPS method to 1047 Sun-like stars observed by the Kepler telescope. We considered two stellar samples individually: one with near-solar rotation periods (24-27.4 d) and a broad range of effective temperatures (5000-6000 K) and the other with near-solar effective temperatures (5700-5900 K) and a broad range of rotation periods (15-40 d).
Results: We show that the GPS method returns precise values for stellar rotation periods. Furthermore, it allows us to constrain the ratio between facular and spot areas of active regions at the moment of their emergence. We also show that the relative facular area decreases with the stellar rotation rate.
Conclusions: Our results suggest that the GPS method can be successfully applied to retrieve the periods of stars with both regular and non-regular light curves.

Full Table 2 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/642/A225 Title: Solar Irradiance Variability: Modeling the Measurements Authors: Lean, J. L.; Coddington, O.; Marchenko, S. V.; Machol, J.; DeLand, M. T.; Kopp, G. Bibcode: 2020E&SS....700645L Altcode: New models of the Sun's irradiance variability are developed from 15 years of direct observations made by the Solar Radiation and Climate Experiment (SORCE) spacecraft from 2003 to 2017 (inclusive). Multiple linear regression parameterizes the observations in terms of facular brightening and sunspot darkening, which are the primary sources of solar irradiance variability. The facular influence is specified as a combination of a linear and nonlinear solar ultraviolet (UV) index; the addition of the nonlinear term allows better reproduction of concurrent solar cycle and rotational variability. The sunspot darkening index is calculated using sunspot observations from both the Debrecen catalog and Air Force Solar Observing Optical Network (SOON) operational sites, the former providing superior model performance. The new model of total solar irradiance variability, NRLTSI3, with the Debrecen sunspot index reproduces the direct Total Irradiance Monitor (TIM) observations better than does the NRLTSI2 model that currently specifies irradiance for the NOAA Climate Data Record (CDR); the correlation of the model and observations increases from 0.956 to 0.971, and the standard deviation of the residuals decreases from 0.124 to 0.100 W m-2. The new model of solar spectral irradiance variability, NRLSSI3, which extends from 115 to 100,000 nm, reproduces rotational modulation in independent Ozone Monitoring Instrument (OMI) observations at near-UV and visible wavelengths. The SATIRE model overestimates rotational modulation of near-UV Fraunhofer spectral features because of excess facular brightness; the EMPIRE model overestimates rotational modulation at all near-UV wavelengths. Title: Changing of the Guard for the Total Solar Irradiance Record Authors: Kopp, Greg; Harber, David; Heuerman, Karl; Stone, Brandon Bibcode: 2020EGUGA..2211489K Altcode: The uninterrupted, 41-year-long, spaceborne total solar irradiance (TSI) record has recently undergone several changes in the instruments contributing to these measurements of the net incoming radiant energy providing nearly all the power driving the Earth's climate system. Two long-term instruments, NASA's SORCE/TIM and TCTE/TIM, have recently been powered off. This ends the 17-year record from the SORCE/TIM, which established the currently-accepted TSI value of 1361 W m-2 after its launch in 2003. ESA's SoHO/VIRGO continues to acquire measurements that extend its 24-year record, but data availability has been on hold as a new processing methodology is implemented. NASA's recently-launched TSIS-1/TIM is presently continuing the measurements of these stalwart legacy instruments. This new TSI instrument is demonstrating higher on-orbit accuracy than any prior such instrument has achieved, with daily measurement updates that are available to the community for climate- and solar-research purposes. I will discuss the many recent changes to the spaceborne TSI measurement record, the current measurement-accuracy improvements and stabilities achieved and their implications for Earth energy-balance studies, and the future plans to maintain measurement continuity. Title: Inflection point in the power spectrum of stellar brightness variations. II. The Sun Authors: Amazo-Gómez, E. M.; Shapiro, A. I.; Solanki, S. K.; Krivova, N. A.; Kopp, G.; Reinhold, T.; Oshagh, M.; Reiners, A. Bibcode: 2020A&A...636A..69A Altcode: 2020arXiv200203455A Context. Young and active stars generally have regular, almost sinusoidal, patterns of variability attributed to their rotation, while the majority of older and less active stars, including the Sun, have more complex and non-regular light curves, which do not have clear rotational-modulation signals. Consequently, the rotation periods have been successfully determined only for a small fraction of the Sun-like stars (mainly the active ones) observed by transit-based planet-hunting missions, such as CoRoT, Kepler, and TESS. This suggests that only a small fraction of such systems have been properly identified as solar-like analogues.
Aims: We aim to apply a new method of determining rotation periods of low-activity stars, such as the Sun. The method is based on calculating the gradient of the power spectrum (GPS) of stellar brightness variations and identifying a tell-tale inflection point in the spectrum. The rotation frequency is then proportional to the frequency of that inflection point. In this paper, we compare this GPS method to already-available photometric records of the Sun.
Methods: We applied GPS, auto-correlation functions, Lomb-Scargle periodograms, and wavelet analyses to the total solar irradiance (TSI) time series obtained from the Total Irradiance Monitor on the Solar Radiation and Climate Experiment and the Variability of solar IRradiance and Gravity Oscillations experiment on the SOlar and Heliospheric Observatory missions. We analysed the performance of all methods at various levels of solar activity.
Results: We show that the GPS method returns accurate values of solar rotation independently of the level of solar activity. In particular, it performs well during periods of high solar activity, when TSI variability displays an irregular pattern, and other methods fail. Furthermore, we show that the GPS and light curve skewness can give constraints on facular and spot contributions to brightness variability.
Conclusions: Our results suggest that the GPS method can successfully determine the rotational periods of stars with both regular and non-regular light curves.

The two movies are available at https://www.aanda.org Title: SiPM-matrix readout of two-phase argon detectors using electroluminescence in the visible and near infrared range Authors: The DarkSide collaboration; Aalseth, C. E.; Abdelhakim, S.; Agnes, P.; Ajaj, R.; Albuquerque, I. F. M.; Alexander, T.; Alici, A.; Alton, A. K.; Amaudruz, P.; Ameli, F.; Anstey, J.; Antonioli, P.; Arba, M.; Arcelli, S.; Ardito, R.; Arnquist, I. J.; Arpaia, P.; Asner, D. M.; Asunskis, A.; Ave, M.; Back, H. O.; Barbaryan, V.; Barrado Olmedo, A.; Batignani, G.; Bisogni, M. G.; Bocci, V.; Bondar, A.; Bonfini, G.; Bonivento, W.; Borisova, E.; Bottino, B.; Boulay, M. G.; Bunker, R.; Bussino, S.; Buzulutskov, A.; Cadeddu, M.; Cadoni, M.; Caminata, A.; Canci, N.; Candela, A.; Cantini, C.; Caravati, M.; Cariello, M.; Carnesecchi, F.; Castellani, A.; Castello, P.; Cavalcante, P.; Cavazza, D.; Cavuoti, S.; Cebrian, S.; Cela Ruiz, J. M.; Celano, B.; Cereseto, R.; Chashin, S.; Cheng, W.; Chepurnov, A.; Cicalò, C.; Cifarelli, L.; Citterio, M.; Coccetti, F.; Cocco, V.; Colocci, M.; Conde Vilda, E.; Consiglio, L.; Cossio, F.; Covone, G.; Crivelli, P.; D'Antone, I.; D'Incecco, M.; Da Rocha Rolo, M. D.; Dadoun, O.; Daniel, M.; Davini, S.; De Cecco, S.; De Deo, M.; De Falco, A.; De Gruttola, D.; De Guido, G.; De Rosa, G.; Dellacasa, G.; Demontis, P.; De Pasquale, S.; Derbin, A. V.; Devoto, A.; Di Eusanio, F.; Di Noto, L.; Di Pietro, G.; Di Stefano, P.; Dionisi, C.; Dolganov, G.; Dordei, F.; Downing, M.; Edalatfar, F.; Empl, A.; Fernandez Diaz, M.; Filip, C.; Fiorillo, G.; Fomenko, K.; Franceschi, A.; Franco, D.; Frolov, E.; Froudakis, G. E.; Funicello, N.; Gabriele, F.; Gabrieli, A.; Galbiati, C.; Garbini, M.; Garcia Abia, P.; Gascón Fora, D.; Gendotti, A.; Ghiano, C.; Ghisi, A.; Giampa, P.; Giampaolo, R. A.; Giganti, C.; Giorgi, M. A.; Giovanetti, G. K.; Gligan, M. L.; Gorchakov, O.; Grab, M.; Graciani Diaz, R.; Grassi, M.; Grate, J. W.; Grobov, A.; Gromov, M.; Guan, M.; Guerra, M. B. B.; Guerzoni, M.; Gulino, M.; Haaland, R. K.; Hackett, B. R.; Hallin, A.; Haranczyk, M.; Harrop, B.; Hoppe, E. W.; Horikawa, S.; Hosseini, B.; Hubaut, F.; Humble, P.; Hungerford, E. V.; Ianni, An.; Ilyasov, A.; Ippolito, V.; Jillings, C.; Keeter, K.; Kendziora, C. L.; Kochanek, I.; Kondo, K.; Kopp, G.; Korablev, D.; Korga, G.; Kubankin, A.; Kugathasan, R.; Kuss, M.; La Commara, M.; La Delfa, L.; Lai, M.; Lebois, M.; Lehnert, B.; Levashko, N.; Li, X.; Liqiang, Q.; Lissia, M.; Lodi, G. U.; Longo, G.; Lussana, R.; Luzzi, L.; Machado, A. A.; Machulin, I. N.; Mandarano, A.; Manecki, S.; Mapelli, L.; Margotti, A.; Mari, S. M.; Mariani, M.; Maricic, J.; Marinelli, M.; Marras, D.; Martínez, M.; Martinez Rojas, A. D.; Mascia, M.; Mason, J.; Masoni, A.; McDonald, A. B.; Messina, A.; Miletic, T.; Milincic, R.; Moggi, A.; Moioli, S.; Monroe, J.; Morrocchi, M.; Mroz, T.; Mu, W.; Muratova, V. N.; Murphy, S.; Muscas, C.; Musico, P.; Nania, R.; Napolitano, T.; Navrer Agasson, A.; Nessi, M.; Nikulin, I.; Nosov, V.; Nowak, J. A.; Oleinik, A.; Oleynikov, V.; Orsini, M.; Ortica, F.; Pagani, L.; Pallavicini, M.; Palmas, S.; Pandola, L.; Pantic, E.; Paoloni, E.; Pazzona, F.; Peeters, S.; Pegoraro, P. A.; Pelczar, K.; Pellegrini, L. A.; Pellegrino, C.; Pelliccia, N.; Perotti, F.; Pesudo, V.; Picciau, E.; Pietropaolo, F.; Pocar, A.; Pollmann, T. R.; Portaluppi, D.; Poudel, S. S.; Pralavorio, P.; Price, D.; Radics, B.; Raffaelli, F.; Ragusa, F.; Razeti, M.; Regenfus, C.; Renshaw, A. L.; Rescia, S.; Rescigno, M.; Retiere, F.; Rignanese, L. P.; Ripoli, C.; Rivetti, A.; Rode, J.; Romani, A.; Romero, L.; Rossi, N.; Rubbia, A.; Sala, P.; Salatino, P.; Samoylov, O.; Sánchez García, E.; Sandford, E.; Sanfilippo, S.; Sant, M.; Santone, D.; Santorelli, R.; Savarese, C.; Scapparone, E.; Schlitzer, B.; Scioli, G.; Segreto, E.; Seifert, A.; Semenov, D. A.; Shchagin, A.; Sheshukov, A.; Siddhanta, S.; Simeone, M.; Singh, P. N.; Skensved, P.; Skorokhvatov, M. D.; Smirnov, O.; Sobrero, G.; Sokolov, A.; Sotnikov, A.; Stainforth, R.; Steri, A.; Stracka, S.; Strickland, V.; Suffritti, G. B.; Sulis, S.; Suvorov, Y.; Szelc, A. M.; Tartaglia, R.; Testera, G.; Thorpe, T.; Tonazzo, A.; Tosi, A.; Tuveri, M.; Unzhakov, E. V.; Usai, G.; Vacca, A.; Vázquez-Jáuregui, E.; Viant, T.; Viel, S.; Villa, F.; Vishneva, A.; Vogelaar, R. B.; Wahl, J.; Walding, J. J.; Wang, H.; Wang, Y.; Westerdale, S.; Wheadon, R. J.; Williams, R.; Wilson, J.; Wojcik, Ma. M.; Wojcik, Ma.; Wu, S.; Xiao, X.; Yang, C.; Ye, Z.; Zuffa, M.; Zuzel, G. Bibcode: 2020arXiv200402024T Altcode: Proportional electroluminescence (EL) in noble gases is used in two-phase detectors for dark matter searches to record (in the gas phase) the ionization signal induced by particle scattering in the liquid phase. The "standard" EL mechanism is considered to be due to noble gas excimer emission in the vacuum ultraviolet (VUV). In addition, there are two alternative mechanisms, producing light in the visible and near infrared (NIR) ranges. The first is due to bremsstrahlung of electrons scattered on neutral atoms ("neutral bremsstrahlung", NBrS). The second, responsible for electron avalanche scintillation in the NIR at higher electric fields, is due to transitions between excited atomic states. In this work, we have for the first time demonstrated two alternative techniques of the optical readout of two-phase argon detectors, in the visible and NIR range, using a silicon photomultiplier matrix and electroluminescence due to either neutral bremsstrahlung or avalanche scintillation. The amplitude yield and position resolution were measured for these readout techniques, which allowed to assess the detection threshold for electron and nuclear recoils in two-phase argon detectors for dark matter searches. To the best of our knowledge, this is the first practical application of the NBrS effect in detection science. Title: Solar Irradiance: Instrument-Based Advances Authors: Kopp, Greg Bibcode: 2020IAUGA..30..354K Altcode: Variations of the total solar irradiance (TSI) over long periods of time provide natural Earth-climate forcing and are thus important to monitor. Variations over a solar cycle are at the 0.1 % level. Variations on multi-decadal to century timescales are (fortunately for our climate stability) very small, which drives the need for highly-accurate and stable measurements over correspondingly long periods of time to discern any such irradiance changes. Advances to TSI-measuring space-borne instruments are approaching the desired climate-driven measurement accuracies and on-orbit stabilities. I present a summary of the modern-instrument improvements enabling these measurements and present some of the solar-variability measurement results from recent space-borne instruments, including TSI variations on timescales from solar flares and large-scale convection to solar cycles. Title: First TSI results and status report of the CLARA/NorSat-1 solar absolute radiometer Authors: Walter, Benjamin; Andersen, Bo; Beattie, Alexander; Finsterle, Wolfgang; Kopp, Greg; Pfiffner, Daniel; Schmutz, Werner Bibcode: 2020IAUGA..30..358W Altcode: The Compact Lightweight Absolute Radiometer (CLARA) is orbiting Earth on-board the Norwegian NorSat-1 micro-satellite since 14th of July 2017. The first light total solar irradiance (TSI) measurement result of CLARA is 1360.18 W m-2 for the so far single reliable Channel B. Channel A and C measured significantly lower (higher) TSI values and were found being sensitive to satellite pointing instabilities. These channels most likely suffer from electrical interference between satellite components and CLARA, an effect that is currently under investigation. Problems with the satellite attitude control currently inhibit stable pointing of CLARA to the Sun. Title: Solar irradiance: from multiple observations to a single composite Authors: Dudok de Wit, Thierry; Kopp, Greg Bibcode: 2020IAUGA..30..336D Altcode: We review recent developments in combining solar irradiance datasets from different instruments to obtain one single composite, which is the key to understanding how irradiance varies on decadal timescales and beyond. Title: FM9 - Solar Irradiance: Physics-Based Advances Authors: Kopp, Greg; Shapiro, Alexander Bibcode: 2020IAUGA..30..331K Altcode: No abstract at ADS Title: Design and construction of a new detector to measure ultra-low radioactive-isotope contamination of argon Authors: Aalseth, C. E.; Abdelhakim, S.; Acerbi, F.; Agnes, P.; Ajaj, R.; Albuquerque, I. F. M.; Alexander, T.; Alici, A.; Alton, A. K.; Amaudruz, P.; Ameli, F.; Anstey, J.; Antonioli, P.; Arba, M.; Arcelli, S.; Ardito, R.; Arnquist, I. J.; Arpaia, P.; Asner, D. M.; Asunskis, A.; Ave, M.; Back, H. O.; Barbaryan, V.; Barrado Olmedo, A.; Batignani, G.; Bisogni, M. G.; Bocci, V.; Bondar, A.; Bonfini, G.; Bonivento, W.; Borisova, E.; Bottino, B.; Boulay, M. G.; Bunker, R.; Bussino, S.; Buzulutskov, A.; Cadeddu, M.; Cadoni, M.; Caminata, A.; Canci, N.; Candela, A.; Cantini, C.; Caravati, M.; Cariello, M.; Carnesecchi, F.; Carpinelli, M.; Castellani, A.; Castello, P.; Catalanotti, S.; Cataudella, V.; Cavalcante, P.; Cavazza, D.; Cavuoti, S.; Cebrian, S.; Cela Ruiz, J. M.; Celano, B.; Cereseto, R.; Cheng, W.; Chepurnov, A.; Cicalò, C.; Cifarelli, L.; Citterio, M.; Coccetti, F.; Cocco, A. G.; Cocco, V.; Colocci, M.; Consiglio, L.; Cossio, F.; Covone, G.; Crivelli, P.; D'Antone, I.; D'Incecco, M.; D'Urso, D.; Da Rocha Rolo, M. D.; Dadoun, O.; Daniel, M.; Davini, S.; De Candia, A.; De Cecco, S.; De Deo, M.; De Falco, A.; De Filippis, G.; De Gruttola, D.; De Guido, G.; De Rosa, G.; Dellacasa, G.; Demontis, P.; DePaquale, S.; Derbin, A. V.; Devoto, A.; Di Eusanio, F.; Di Noto, L.; Di Pietro, G.; Di Stefano, P.; Dionisi, C.; Dolganov, G.; Dordei, F.; Downing, M.; Edalatfar, F.; Empl, A.; Fernandez Diaz, M.; Ferri, A.; Filip, C.; Fiorillo, G.; Fomenko, K.; Franceschi, A.; Franco, D.; Froudakis, G. E.; Gabriele, F.; Gabrieli, A.; Galbiati, C.; Garbini, M.; Garcia Abia, P.; Gascón Fora, D.; Gendotti, A.; Ghiano, C.; Ghisi, A.; Giagu, S.; Giampa, P.; Giampaolo, R. A.; Giganti, C.; Giorgi, M. A.; Giovanetti, G. K.; Gligan, M. L.; Gola, A.; Gorchakov, O.; Grab, M.; Graciani Diaz, R.; Granato, F.; Grassi, M.; Grate, J. W.; Grigoriev, G. Y.; Grobov, A.; Gromov, M.; Guan, M.; Guerra, M. B. B.; Guerzoni, M.; Gulino, M.; Haaland, R. K.; Hackett, B. R.; Hallin, A.; Harrop, B.; Hoppe, E. W.; Horikawa, S.; Hosseini, B.; Hubaut, F.; Humble, P.; Hungerford, E. V.; Ianni, An.; Ilyasov, A.; Ippolito, V.; Jillings, C.; Keeter, K.; Kendziora, C. L.; Kim, S.; Kochanek, I.; Kondo, K.; Kopp, G.; Korablev, D.; Korga, G.; Kubankin, A.; Kugathasan, R.; Kuss, M.; Kuźniak, M.; La Commara, M.; La Delfa, L.; Lai, M.; Langrock, S.; Lebois, M.; Lehnert, B.; Levashko, N.; Li, X.; Liqiang, Q.; Lissia, M.; Lodi, G. U.; Longo, G.; López Manzano, R.; Lussana, R.; Luzzi, L.; Machado, A. A.; Machulin, I. N.; Mandarano, A.; Mapelli, L.; Marcante, M.; Margotti, A.; Mari, S. M.; Mariani, M.; Maricic, J.; Marinelli, M.; Marras, D.; Martínez, M.; Martínez Morales, J. J.; Martinez Rojas, A. D.; Martoff, C. J.; Mascia, M.; Mason, J.; Masoni, A.; Mazzi, A.; McDonald, A. B.; Messina, A.; Meyers, P. D.; Miletic, T.; Milincic, R.; Moggi, A.; Moioli, S.; Monroe, J.; Morrocchi, M.; Mroz, T.; Mu, W.; Muratova, V. N.; Murphy, S.; Muscas, C.; Musico, P.; Nania, R.; Napolitano, T.; Navrer Agasson, A.; Nessi, M.; Nikulin, I.; Oleinik, A.; Oleynikov, V.; Orsini, M.; Ortica, F.; Pagani, L.; Pallavicini, M.; Palmas, S.; Pandola, L.; Pantic, E.; Paoloni, E.; Paternoster, G.; Pazzona, F.; Peeters, S.; Pegoraro, P. A.; Pelczar, K.; Pellegrini, L. A.; Pellegrino, C.; Pelliccia, N.; Perotti, F.; Pesudo, V.; Picciau, E.; Piemonte, C.; Pietropaolo, F.; Pocar, A.; Pollmann, T. R.; Portaluppi, D.; Poudel, S. S.; Pralavorio, P.; Price, D.; Radics, B.; Raffaelli, F.; Ragusa, F.; Razeti, M.; Razeto, A.; Regazzoni, V.; Regenfus, C.; Renshaw, A. L.; Rescia, S.; Rescigno, M.; Retiere, F.; Rignanese, L. P.; Rivetti, A.; Romani, A.; Romero, L.; Rossi, N.; Rubbia, A.; Sablone, D.; Sala, P.; Salatino, P.; Samoylov, O.; Sánchez García, E.; Sanfilippo, S.; Sant, M.; Santone, D.; Santorelli, R.; Savarese, C.; Scapparone, E.; Schlitzer, B.; Scioli, G.; Segreto, E.; Seifert, A.; Semenov, D. A.; Shchagin, A.; Sheshukov, A.; Siddhanta, S.; Simeone, M.; Singh, P. N.; Skensved, P.; Skorokhvatov, M. D.; Smirnov, O.; Sobrero, G.; Sokolov, A.; Sotnikov, A.; Stainforth, R.; Steri, A.; Stracka, S.; Strickland, V.; Suffritti, G. B.; Sulis, S.; Suvorov, Y.; Szelc, A. M.; Tartaglia, R.; Testera, G.; Thorpe, T.; Tonazzo, A.; Tosi, A.; Tuveri, M.; Unzhakov, E. V.; Usai, G.; Vacca, A.; Vázquez-Jáuregui, E.; Verducci, M.; Viant, T.; Viel, S.; Villa, F.; Vishneva, A.; Vogelaar, R. B.; Wada, M.; Wahl, J.; Walding, J. J.; Wang, H.; Wang, Y.; Westerdale, S.; Wheadon, R. J.; Williams, R.; Wilson, J.; Wojcik, Marcin; Wojcik, Mariusz; Wu, S.; Xiao, X.; Yang, C.; Ye, Z.; Zuffa, M.; Zuzel, G. Bibcode: 2020JInst..15P2024A Altcode: 2020arXiv200108106T Large liquid argon detectors offer one of the best avenues for the detection of galactic weakly interacting massive particles (WIMPs) via their scattering on atomic nuclei. The liquid argon target allows exquisite discrimination between nuclear and electron recoil signals via pulse-shape discrimination of the scintillation signals. Atmospheric argon (AAr), however, has a naturally occurring radioactive isotope, 39Ar, a β emitter of cosmogenic origin. For large detectors, the atmospheric 39Ar activity poses pile-up concerns. The use of argon extracted from underground wells, deprived of 39Ar, is key to the physics potential of these experiments. The DarkSide-20k dark matter search experiment will operate a dual-phase time projection chamber with 50 tonnes of radio-pure underground argon (UAr), that was shown to be depleted of 39Ar with respect to AAr by a factor larger than 1400. Assessing the 39Ar content of the UAr during extraction is crucial for the success of DarkSide-20k, as well as for future experiments of the Global Argon Dark Matter Collaboration (GADMC). This will be carried out by the DArT in ArDM experiment, a small chamber made with extremely radio-pure materials that will be placed at the centre of the ArDM detector, in the Canfranc Underground Laboratory (LSC) in Spain. The ArDM LAr volume acts as an active veto for background radioactivity, mostly γ-rays from the ArDM detector materials and the surrounding rock. This article describes the DArT in ArDM project, including the chamber design and construction, and reviews the background required to achieve the expected performance of the detector. Title: Overview of the NASA Solar Irradiance Science Team (SIST) Program Special Section Authors: DeLand, Matthew T.; Kopp, Greg; Considine, David B. Bibcode: 2019E&SS....6.2229D Altcode: Solar irradiance represents the dominant energy source heating the Earth's atmosphere and climate. Both total solar irradiance and spectral solar irradiance vary over the 11-year solar cycle. Characterizing these variations with sufficient accuracy for climate studies over multidecadal timescales requires a combination of multiple observational data sets, solar activity proxies, and irradiance models. NASA established the Solar Irradiance Science Team (SIST) program in 2015 to pursue this goal using a range of technical approaches. This paper summarizes those investigations, whose results are reported in separate papers in a special section of this journal. Title: Solar Irradiance Variability: Comparisons of Models and Measurements Authors: Coddington, O.; Lean, J.; Pilewskie, P.; Snow, M.; Richard, E.; Kopp, G.; Lindholm, C.; DeLand, M.; Marchenko, S.; Haberreiter, M.; Baranyi, T. Bibcode: 2019E&SS....6.2525C Altcode: The Earth system responds to solar variability on a wide range of timescales. Knowledge of total solar irradiance (TSI) and solar spectral irradiance (SSI) spanning minutes to centuries is needed by scientists studying a broad array of research applications. For these purposes, the NOAA National Centers for Environmental Information (NCEI) Climate Data Record Program established the Solar Irradiance Climate Data Record. Version 2 of the Naval Research Laboratory's solar variability models that are derived from and demonstrate consistency with irradiance observations specifies TSI and SSI for the Solar Irradiance Climate Data Record. We establish the veracity of the Naval Research Laboratory models on the timescales and over the wavelength range for which the Sun is known to vary and, thereby, specify the utility of these models. Through comparisons with irradiance observations and independent models, we validate NRLTSI2 estimates of TSI on solar rotational (~27-day), solar cycle (~11-year), and multidecadal (spacecraft era) variability timescales. Similarly, we validate NRLSSI2 estimates of SSI rotational variability in the ultraviolet through the mid-visible spectrum. Validation of NRLSSI2 estimates at longer wavelengths, particularly in the near-infrared, and for the full spectrum at solar cycle timescales and longer is not possible with the current observational record due to instrumental noise and instrument instability. We identify where key new data sets, such as observations from the Total and Spectral Solar Irradiance Sensor-1, are expected to provide a fuller understanding of total and spectral solar irradiance variability on multiple timescales. Title: Compact total irradiance monitor flight demonstration Authors: Harber, David; Castleman, Zach; Drake, Ginger; Van Dreser, Samuel; Farber, Nat; Heuerman, Karl; Miller, Marc; Rutkowski, Joel; Sims, Alan; Sprunck, Jacob; Straatsma, Cameron; Wanamaker, Isaac; Zheng, Wengang; Kopp, Greg; Richard, Erik; Pilewskie, Peter; Tomlin, Nathan; Stephens, Michelle; Yung, Christopher; White, Malcolm; Lehman, John Bibcode: 2019SPIE11131E..0DH Altcode: The long-term balance between Earth's absorption of solar energy and emission of radiation to space is a fundamental climate measurement. Total solar irradiance (TSI) has been measured from space, uninterrupted, for the past 40 years via a series of instruments. The Compact Total Irradiance Monitor (CTIM) is a CubeSat instrument that will demonstrate next-generation technology for monitoring total solar irradiance. It includes novel silicon-substrate room temperature vertically aligned carbon nanotube (VACNT) bolometers. The CTIM, an eight-channel 6U CubeSat instrument, is being built for a target launch date in late 2020. The basic design is similar to the SORCE, TCTE and TSIS Total Irradiance Monitors (TIM). Like TSIS TIM, it will measure the total irradiance of the Sun with an uncertainty of 0.0097% and a stability of <0.001%/year. The underlying technology, including the silicon substrate VACNT bolometers, has been demonstrated at the prototype-level. During 2019 we will build and test an engineering model of the detector subsystem. Following the testing of the engineering detector subsystem, we will build a flight detector unit and integrate it with a 6U CubeSat bus during late 2019 and 2020, in preparation for an on-orbit demonstration in 2021. Title: GPS, decrypting brightness variations of the Sun and Sun-like Authors: Amazo-Gómez, Eliana Maritza; Shapiro, Alexander I.; Solanki, Sami K.; Kopp, Greg; Oshagh, Mahmoudreza; Reinhold, Timo; Krivova, Natalie A.; Reiners, Ansgar Bibcode: 2019shin.confE.109A Altcode: The rotation period is in general detectable in the light curves of young and active stars. Even after successful stellar surveys stemmed from Kepler mission, there is still a lack of information in photometric records of rotation periods in Sun-like stars. Non-periodic light-curve profiles, low variability contrast -therefore low modulation amplitude- short lifetime evolution and random emergence of magnetic features (in comparison to the rotation time-scale) are the main reasons of unreliable determination of rotation periodicity in the Sun and its closer analogs. This indicates that only a small fraction of solar-like systems have been properly analyzed. We show that the rotation periods of those stars can be reliably determined from the profile of the gradient of the power spectra, GPS. By analysing periodic patterns in high-accuracy measurements of the total solar irradiance, TSI, by SORCE/TIM and SoHO/VIRGO missions, here we test and validate GPS, linking the variability by transits of magnetic features over the stellar surface with a clear and enhanced signal of the solar rotation. GPS method retrieves accurate and stable values of rotation period during different regimes of solar activity cycle and could be applied to stars of comparable and higher activity - where other methods underperform. Furthermore, GPS gives us constraints on the faculae to spot driver ratio and consequently help us to interpret the stellar surface. Title: Response of Solar Irradiance to Sunspot-area Variations Authors: Dudok de Wit, T.; Kopp, G.; Shapiro, A.; Witzke, V.; Kretzschmar, M. Bibcode: 2018ApJ...853..197D Altcode: 2018arXiv180504350D One of the important open questions in solar irradiance studies is whether long-term variability (i.e., on timescales of years and beyond) can be reconstructed by means of models that describe short-term variability (i.e., days) using solar proxies as inputs. Preminger & Walton showed that the relationship between spectral solar irradiance and proxies of magnetic-flux emergence, such as the daily sunspot area, can be described in the framework of linear system theory by means of the impulse response. We significantly refine that empirical model by removing spurious solar-rotational effects and by including an additional term that captures long-term variations. Our results show that long-term variability cannot be reconstructed from the short-term response of the spectral irradiance, which questions the extension of solar proxy models to these timescales. In addition, we find that the solar response is nonlinear in a way that cannot be corrected simply by applying a rescaling to a sunspot area. Title: A New Revision of the Solar Irradiance Climate Data Record Incorporates Recent Research into Proxies of Sunspot Darkening and the Sunspot Number Record Authors: Coddington, O.; Lean, J.; Pilewskie, P.; Baranyi, T.; Snow, M. A.; Kopp, G.; Richard, E. C.; Lindholm, C. Bibcode: 2017AGUFMSH43B2818C Altcode: An operational climate data record (CDR) of total and spectral solar irradiance became available in November 2015 as part of the National Oceanographic and Atmospheric Administration's National Centers for Environmental Information Climate Data Record Program. The data record, which is updated quarterly, is available from 1610 to the present as yearly-average values and from 1882 to the present as monthly- and daily-averages, with associated time and wavelength-dependent uncertainties. It was developed jointly by the University of Colorado at Boulder's Laboratory for Atmospheric and Space Physics and the Naval Research Laboratory, and, together with the source code and supporting documentation, is available at https://www.ncdc.noaa.gov/cdr/. In the Solar Irradiance CDR, total solar irradiance (TSI) and solar spectral irradiance (SSI) are estimated from models that determine the changes from quiet Sun conditions arising from bright faculae and dark sunspots on the solar disk. The models are constructed using linear regression of proxies of solar sunspot and facular features with the approximately decade-long irradiance observations from the SOlar Radiation and Climate Experiment. A new revision of this data record was recently released in an ongoing effort to reduce solar irradiance uncertainties in two ways. First, the sunspot darkening proxy was revised using a new cross calibration of the current sunspot region observations made by the Solar Observing Optical Network with the historical records of the Royal Greenwich Observatory. This implementation affects modeled irradiances from 1882 - 1978. Second, the impact of a revised record of sunspot number by the Sunspot Index and Long-term Solar Observations center on modeled irradiances was assessed. This implementation provides two different reconstructions of historical, yearly-averaged irradiances from 1610-1881. Additionally, we show new, preliminary results that demonstrate improvements in modeled TSI by using Debrecen Photoheliographic sunspot area and location data produced by the Debrecen Heliophysical Observatory as the proxy of sunspot darkening. Our results describe comparisons of the modeled TSI and SSI with observational records and with other solar irradiance models. Title: Methodology to create a new total solar irradiance record: Making a composite out of multiple data records Authors: Dudok de Wit, Thierry; Kopp, Greg; Fröhlich, Claus; Schöll, Micha Bibcode: 2017GeoRL..44.1196D Altcode: 2017arXiv170202341D Many observational records critically rely on our ability to merge different (and not necessarily overlapping) observations into a single composite. We provide a novel and fully traceable approach for doing so, which relies on a multiscale maximum likelihood estimator. This approach overcomes the problem of data gaps in a natural way and uses data-driven estimates of the uncertainties. We apply it to the total solar irradiance (TSI) composite, which is currently being revised and is critical to our understanding of solar radiative forcing. While the final composite is pending decisions on what corrections to apply to the original observations, we find that the new composite is in closest agreement with the PMOD composite and the NRLTSI2 model. In addition, we evaluate long-term uncertainties in the TSI, which reveal a 1/f scaling. Title: How to Establish Traceability for Total Solar Irradiance Data to Ground-Based Standards Authors: Finsterle, W.; Walter, B.; Kopp, G. Bibcode: 2016AGUFMSH31B2557F Altcode: Total Solar Irradiance (TSI) has been measured with radiometers from space continuously since 1978. The observed TSI variations are mostly attributed to the solar activity cycle and longer-term trends are not unambiguously detected in the available TSI record. Nevertheless have such trends likely occurred in the past and are also expected to occur in the future. Because of the dominant role that TSI plays in the Earth's energy budget even small trends are likely to have signficant effects on the climate and the global temperature. In order to detect such trends, the TSI the data from separate radiometers have to be made comparable, ideally through traceability of their measurements to ground-based irradiance standards. We will present how the traceability chain is established for the upcoming CLARA/NORSAT-1 mission and review the traceability of previous TSI measurements. Title: The New Climate Data Record of Solar Irradiance: Comparisons with Observations and Solar Irradiance Models Over a Range of Solar Activity Time Scales Authors: Coddington, O.; Lean, J.; Pilewskie, P.; Richard, E. C.; Snow, M. A.; Kopp, G.; Lindholm, C. Bibcode: 2016AGUFMSA54A..02C Altcode: A new publically available climate data record (CDR) of total and spectral solar irradiance became operational in November 2015 as part of the National Oceanographic and Atmospheric Administration's (NOAA's) National Centers for Environmental Information (NCEI) Climate Data Record Program. The data record, which is updated regularly, is available from 1610 to the present day as yearly-average values and from 1882 to the present day as monthly- and daily-averages, with associated time and wavelength-dependent uncertainties. It was developed jointly by the University of Colorado at Boulder's Laboratory for Atmospheric and Space Physics (LASP) and the Naval Research Laboratory (NRL) and, together with the source code and supporting documentation, is available at https://www.ncdc.noaa.gov/cdr/. Total solar irradiance (TSI) and solar spectral irradiance (SSI) are estimated from models that determine the changes from quiet Sun conditions arising from bright faculae and dark sunspots on the solar disk. The models are constructed using linear regression of proxies of solar sunspot and facular features with the approximately decade-long irradiance observations from the SOlar Radiation and Climate Experiment (SORCE). We describe the model formulation, uncertainty estimates, and validation approach. We present comparisons of the modeled TSI and SSI with observational records and with other solar irradiance models on solar-rotational, solar-cycle, and multi-decadal timescales. We discuss ongoing efforts to improve the irradiance uncertainty estimates arising from model assumptions and the operational approach to make these updated uncertainty estimates publicly available in a future revision of the Solar Irradiance CDR. Title: The Impact of the Revised Sunspot Record on Solar Irradiance Reconstructions Authors: Kopp, G.; Krivova, N.; Wu, C. J.; Lean, J. Bibcode: 2016SoPh..291.2951K Altcode: 2016SoPh..tmp...42K; 2016arXiv160105397K Reliable historical records of the total solar irradiance (TSI) are needed to assess the extent to which long-term variations in the Sun's radiant energy that is incident upon Earth may exacerbate (or mitigate) the more dominant warming in recent centuries that is due to increasing concentrations of greenhouse gases. We investigate the effects that the new Sunspot Index and Long-term Solar Observations (SILSO) sunspot-number time series may have on model reconstructions of the TSI. In contemporary TSI records, variations on timescales longer than about a day are dominated by the opposing effects of sunspot darkening and facular brightening. These two surface magnetic features, retrieved either from direct observations or from solar-activity proxies, are combined in TSI models to reproduce the current TSI observational record. Indices that manifest solar-surface magnetic activity, in particular the sunspot-number record, then enable reconstructing historical TSI. Revisions of the sunspot-number record therefore affect the magnitude and temporal structure of TSI variability on centennial timescales according to the model reconstruction methods that are employed. We estimate the effects of the new SILSO record on two widely used TSI reconstructions, namely the NRLTSI2 and the SATIRE models. We find that the SILSO record has little effect on either model after 1885, but leads to solar-cycle fluctuations with greater amplitude in the TSI reconstructions prior. This suggests that many eighteenth- and nineteenth-century cycles could be similar in amplitude to those of the current Modern Maximum. TSI records based on the revised sunspot data do not suggest a significant change in Maunder Minimum TSI values, and from comparing this era to the present, we find only very small potential differences in the estimated solar contributions to the climate with this new sunspot record. Title: The 2016 Transit of Mercury Observed from Major Solar Telescopes and Satellites Authors: Pasachoff, Jay M.; Schneider, Glenn; Gary, Dale; Chen, Bin; Sterling, Alphonse C.; Reardon, Kevin P.; Dantowitz, Ronald; Kopp, Greg A. Bibcode: 2016DPS....4811705P Altcode: We report observations from the ground and space of the 9 May 2016 transit of Mercury. We build on our explanation of the black-drop effect in transits of Venus based on spacecraft observations of the 1999 transit of Mercury (Schneider, Pasachoff, and Golub, Icarus 168, 249, 2004). In 2016, we used the 1.6-m New Solar Telescope at the Big Bear Solar Observatory with active optics to observe Mercury's transit at high spatial resolution. We again saw a small black-drop effect as 3rd contact neared, confirming the data that led to our earlier explanation as a confluence of the point-spread function and the extreme solar limb darkening (Pasachoff, Schneider, and Golub, in IAU Colloq. 196, 2004). We again used IBIS on the Dunn Solar Telescope of the Sacramento Peak Observatory, as A. Potter continued his observations, previously made at the 2006 transit of Mercury, at both telescopes of the sodium exosphere of Mercury (Potter, Killen, Reardon, and Bida, Icarus 226, 172, 2013). We imaged the transit with IBIS as well as with two RED Epic IMAX-quality cameras alongside it, one with a narrow passband. We show animations of our high-resolution ground-based observations along with observations from XRT on JAXA's Hinode and from NASA's Solar Dynamics Observatory. Further, we report on the limit of the transit change in the Total Solar Irradiance, continuing our interest from the transit of Venus TSI (Schneider, Pasachoff, and Willson, ApJ 641, 565, 2006; Pasachoff, Schneider, and Willson, AAS 2005), using NASA's SORCE/TIM and the Air Force's TCTE/TIM. See http://transitofvenus.info and http://nicmosis.as.arizona.edu.Acknowledgments: We were glad for the collaboration at Big Bear of Claude Plymate and his colleagues of the staff of the Big Bear Solar Observatory. We also appreciate the collaboration on the transit studies of Robert Lucas (Sydney, Australia) and Evan Zucker (San Diego, California). JMP appreciates the sabbatical hospitality of the Division of Geosciences and Planetary Sciences of the California Institute of Technology, and of Prof. Andrew Ingersoll there. The solar observations lead into the 2017 eclipse studies, for which JMP is supported by grants from the NSF AGS and National Geographic CRE. Title: Nominal Values for Selected Solar and Planetary Quantities: IAU 2015 Resolution B3 Authors: Prša, Andrej; Harmanec, Petr; Torres, Guillermo; Mamajek, Eric; Asplund, Martin; Capitaine, Nicole; Christensen-Dalsgaard, Jørgen; Depagne, Éric; Haberreiter, Margit; Hekker, Saskia; Hilton, James; Kopp, Greg; Kostov, Veselin; Kurtz, Donald W.; Laskar, Jacques; Mason, Brian D.; Milone, Eugene F.; Montgomery, Michele; Richards, Mercedes; Schmutz, Werner; Schou, Jesper; Stewart, Susan G. Bibcode: 2016AJ....152...41P Altcode: 2016arXiv160509788P In this brief communication we provide the rationale for and the outcome of the International Astronomical Union (IAU) resolution vote at the XXIXth General Assembly in Honolulu, Hawaii, in 2015, on recommended nominal conversion constants for selected solar and planetary properties. The problem addressed by the resolution is a lack of established conversion constants between solar and planetary values and SI units: a missing standard has caused a proliferation of solar values (e.g., solar radius, solar irradiance, solar luminosity, solar effective temperature, and solar mass parameter) in the literature, with cited solar values typically based on best estimates at the time of paper writing. As precision of observations increases, a set of consistent values becomes increasingly important. To address this, an IAU Working Group on Nominal Units for Stellar and Planetary Astronomy formed in 2011, uniting experts from the solar, stellar, planetary, exoplanetary, and fundamental astronomy, as well as from general standards fields to converge on optimal values for nominal conversion constants. The effort resulted in the IAU 2015 Resolution B3, passed at the IAU General Assembly by a large majority. The resolution recommends the use of nominal solar and planetary values, which are by definition exact and are expressed in SI units. These nominal values should be understood as conversion factors only, not as the true solar/planetary properties or current best estimates. Authors and journal editors are urged to join in using the standard values set forth by this resolution in future work and publications to help minimize further confusion. Title: Magnitudes and timescales of total solar irradiance variability Authors: Kopp, Greg Bibcode: 2016JSWSC...6A..30K Altcode: 2016arXiv160605258K The Sun's net radiative output varies on timescales of minutes to gigayears. Direct measurements of the total solar irradiance (TSI) show changes in the spatially- and spectrally-integrated radiant energy on timescales as short as minutes to as long as a solar cycle. Variations of ~0.01% over a few minutes are caused by the ever-present superposition of convection and oscillations with very large solar flares on rare occasion causing slightly-larger measurable signals. On timescales of days to weeks, changing photospheric magnetic activity affects solar brightness at the ~0.1% level. The 11-year solar cycle shows variations of comparable magnitude with irradiances peaking near solar maximum. Secular variations are more difficult to discern, being limited by instrument stability and the relatively short duration of the space-borne record. Historical reconstructions of the Sun's irradiance based on indicators of solar-surface magnetic activity, such as sunspots, faculae, and cosmogenic isotope records, suggest solar brightness changes over decades to millennia, although the magnitudes of these variations have high uncertainties due to the indirect historical records on which they rely. Stellar evolution affects yet longer timescales and is responsible for the greatest solar variabilities. In this manuscript I summarize the Sun's variability magnitudes over different temporal regimes and discuss the irradiance record's relevance for solar and climate studies as well as for detections of exo-solar planets transiting Sun-like stars. Title: The Next Spaceflight Solar Irradiance Sensor: TSIS Authors: Kopp, Greg; Pilewskie, Peter; Richard, Erik Bibcode: 2016SPD....47.0809K Altcode: The Total and Spectral Solar Irradiance Sensor (TSIS) will continue measurements of the solar irradiance with improved accuracies and stabilities over extant spaceflight instruments. The two TSIS solar-observing instruments include the Total Irradiance Monitor (TIM) and the Spectral Irradiance Monitor (SIM) for measuring total- and spectral- solar-irradiance, respectively. The former provides the net energy powering the Earth’s climate system while the latter helps attribute where that energy is absorbed by the Earth’s atmosphere and surface. Both spaceflight instruments are assembled and being prepared for integration on the International Space Station. With operations commencing in late 2017, the TSIS is intended to overlap with NASA’s ongoing SOlar Radiation and Climate Experiment (SORCE) mission, which launched in 2003 and contains the first versions of both the TIM and SIM instruments, as well as with the TSI Calibration Transfer Experiment (TCTE), which began total solar irradiance measurements in 2013. We summarize the TSIS’s instrument improvements and intended solar-irradiance measurements. Title: The Impact of the Revised Sunspot Record on Solar Irradiance Reconstructions Authors: Kopp, G.; Krivova, N.; Lean, J.; Wu, C. J. Bibcode: 2015AGUFMSH23C2451K Altcode: We describe the expected effects of the new sunspot number time series on proxy model based reconstructions of the total solar irradiance (TSI), which is largely explained by the opposing effects of dark sunspots and bright faculae. Regressions of indices for facular brightening and sunspot darkening with time series of direct TSI observations during the recent 37-year spacecraft TSI measurement era determine the relative contributions from each. Historical TSI reconstructions are enabled by extending these proxy models back in time prior to the start of the measurement record using a variety of solar activity indices including the sunspot number time series alone prior to 1882. Such reconstructions are critical for Earth climate research, which requires knowledge of the incident energy from the Sun to assess climate sensitivity to the natural influence of solar variability. Two prominent TSI reconstructions that utilize the sunspot record starting in 1610 are the NRLTSI and the SATIRE models. We review the indices that each currently uses and estimate the effects the revised sunspot record has on these reconstructions. Title: Solar Variability Magnitudes and Timescales Authors: Kopp, Greg Bibcode: 2015IAUGA..2251303K Altcode: The Sun’s net radiative output varies on timescales of minutes to many millennia. The former are directly observed as part of the on-going 37-year long total solar irradiance climate data record, while the latter are inferred from solar proxy and stellar evolution models. Since the Sun provides nearly all the energy driving the Earth’s climate system, changes in the sunlight reaching our planet can have - and have had - significant impacts on life and civilizations.Total solar irradiance has been measured from space since 1978 by a series of overlapping instruments. These have shown changes in the spatially- and spectrally-integrated radiant energy at the top of the Earth’s atmosphere from timescales as short as minutes to as long as a solar cycle. The Sun’s ~0.01% variations over a few minutes are caused by the superposition of convection and oscillations, and even occasionally by a large flare. Over days to weeks, changing surface activity affects solar brightness at the ~0.1% level. The 11-year solar cycle has comparable irradiance variations with peaks near solar maxima.Secular variations are harder to discern, being limited by instrument stability and the relatively short duration of the space-borne record. Proxy models of the Sun based on cosmogenic isotope records and inferred from Earth climate signatures indicate solar brightness changes over decades to millennia, although the magnitude of these variations depends on many assumptions. Stellar evolution affects yet longer timescales and is responsible for the greatest solar variabilities.In this talk I will summarize the Sun’s variability magnitudes over different temporal ranges, showing examples relevant for climate studies as well as detections of exo-solar planets transiting Sun-like stars. Title: The Total Irradiance Monitors Authors: Kopp, Greg Bibcode: 2015IAUGA..2251309K Altcode: The first Total Irradiance Monitor (TIM) launched on NASA’s Solar Radiation and Climate Experiment in 2003 and quickly proved to be the most accurate and stable instrument on orbit for measuring the total solar irradiance (TSI). The TIM’s design improvements over the older classical radiometers helped its selection on many subsequent missions, including NASA’s Glory, NOAA’s TSI Calibration Transfer Experiment, and the series of NASA’s Total and Spectral Solar Irradiance Sensor instruments currently underway. I will summarize the status of and differences between each of the TIMs currently on-orbit or in production. Title: The solar magnetic activity band interaction and instabilities that shape quasi-periodic variability Authors: McIntosh, Scott W.; Leamon, Robert J.; Krista, Larisza D.; Title, Alan M.; Hudson, Hugh S.; Riley, Pete; Harder, Jerald W.; Kopp, Greg; Snow, Martin; Woods, Thomas N.; Kasper, Justin C.; Stevens, Michael L.; Ulrich, Roger K. Bibcode: 2015NatCo...6.6491M Altcode: 2015NatCo...6E6491M Solar magnetism displays a host of variational timescales of which the enigmatic 11-year sunspot cycle is most prominent. Recent work has demonstrated that the sunspot cycle can be explained in terms of the intra- and extra-hemispheric interaction between the overlapping activity bands of the 22-year magnetic polarity cycle. Those activity bands appear to be driven by the rotation of the Sun's deep interior. Here we deduce that activity band interaction can qualitatively explain the `Gnevyshev Gap'--a well-established feature of flare and sunspot occurrence. Strong quasi-annual variability in the number of flares, coronal mass ejections, the radiative and particulate environment of the heliosphere is also observed. We infer that this secondary variability is driven by surges of magnetism from the activity bands. Understanding the formation, interaction and instability of these activity bands will considerably improve forecast capability in space weather and solar activity over a range of timescales. Title: Sorce Observations of Solar Cycles 23 and 24 - What's New? What's Next? Authors: Cahalan, R. F.; Kopp, G.; Pilewskie, P.; Richard, E. C.; Woods, T. N. Bibcode: 2014AGUFMSH21C4131C Altcode: We discuss recent changes in estimates of the Total Solar Irradiance (TSI, formerly "solar constant") and the energy budget. This more accurate value of TSI implies a more accurate estimate of the Sun's luminosity, and lifetime. We highlight the historic closing of the calibration gap between the suite of TSI instruments, due largely to comparisons made with a cryogenic Transfer Radiometer Facility (TRF) located at the University of Colorado, built by UCO/LASP with support from NASA and NIST. The resulting continuous record of TSI promises to be a milestone in improving understanding of the Sun's impact on Earth's climate. Climate models are sensitive not only to TSI, but also to variations in the Spectral Solar Irradiance (SSI), and the vertical profiles of temperature and ozone are especially sensitive to SSI variations. Variations in SSI need further study before they may be considered as firmly established as TSI variations, which themselves remain controversial, despite a strengthening consensus over the SORCE epoch. The TSIS SIM has recently undergone comprehensive end-to-end calibration in the LASP SSI Radiometry Facility (SRF) utilizing the NIST SIRCUS laser system covering 210-2400 nm for SSI, a facility not yet available when SORCE launched in 2003. With SORCE follow-on missions such as the Total and Spectral Solar Irradiance Sensor (TSIS), we anticipate narrowing uncertainties in SSI variability that will be important to improving our understanding of the climate responses to solar forcing. The long-term goal of improving the ability to monitor Earth's energy balance, and the energy imbalance that drives global warming, will need continued improvements in the measurement of both shortwave solar and longwave earth-emitted radiation. Title: White-Light Observations of Major Flares Compared to Total Solar Irradiance and Short-Wavelength Observations Authors: Petrie, Gordon; Kopp, Greg; Harvey, J. W. Bibcode: 2014AAS...22412327P Altcode: The NSO’s GONG network produces “white light” (WL) continuum intensity images from one-minute integrations averaged across a 0. Å wide band pass centered at 676 Å at one minute cadence using six sites worldwide. Clear WL signatures of solar flares are present in GONG intensity data for only the largest flares because of low spatial resolution (2.5 arcsec pixel size). For six major flares (GOES class X6.5 - X28) observed by GONG, we compare integrated GONG full-disk WL intensity curves with SORCE/TIM total solar irradiance (TSI) measurements. Distinctive p-mode signatures are evident in both GONG and SORCE time series, though the correlation between GONG and SORCE data varies from flare to flare. In some cases a clear TSI peak and an interruption of the GONG p-mode pattern accompany the flare. The flare signature is generally weaker in the GONG data, suggesting that most of the TIM flare signal arises from wavelengths shorter than the GONG band pass. The flare kernels nevertheless are clear and last many minutes in the spatially resolved GONG image time series. We also compare the GONG active region intensity observations with shorter-wavelength data. In one case observed by TRACE, the GONG and TRACE WL curves are very similar and the TRACE 160 Å curve shows a significant precursor and a long tail. In most cases the GONG WL and RHESSI 25-100 keV counts appear well correlated in time. This work utilizes GONG data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. Title: An assessment of the solar irradiance record for climate studies Authors: Kopp, Greg Bibcode: 2014JSWSC...4A..14K Altcode: Total solar irradiance, the spatially and spectrally integrated radiant output from the Sun at a mean Sun-Earth distance of 1 astronomical unit, provides nearly all the energy driving the Earth's climate system. Variations in this energy, particularly over long time scales, contribute to changes in Earth's climate and have been linked to historical glaciation and inter-glacial periods as well as having a small effect on more recent global warming. Accurate measurements of solar irradiances require measurements above the Earth's atmosphere. The total solar irradiance spaceborne record began in 1978 and has been uninterrupted since, with over a dozen instruments contributing to the present solar climate data record. I assess the required and achieved accuracies of this record with a focus on its value for climate studies. Title: Three 2012 Transits of Venus: From Earth, Jupiter, and Saturn Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Edelman, E.; Reardon, K.; Widemann, T.; Tanga, P.; Dantowitz, R.; Silverstone, M. D.; Ehrenreich, D.; Vidal-Madjar, A.; Nicholson, P. D.; Willson, R. C.; Kopp, G. A.; Yurchyshyn, V. B.; Sterling, A. C.; Scherrer, P. H.; Schou, J.; Golub, L.; McCauley, P.; Reeves, K. Bibcode: 2013AAS...22131506P Altcode: We observed the 2012 June 6/5 transit seen from Earth (E/ToV), simultaneously with Venus Express and several other spacecraft not only to study the Cytherean atmosphere but also to provide an exoplanet-transit analog. From Haleakala, the whole transit was visible in coronal skies; among our instruments was one of the world-wide Venus Twilight Experiment's nine coronagraphs. Venus's atmosphere became visible before first contact. SacPeak/IBIS provided high-resolution images at Hα/carbon-dioxide. Big Bear's NST also provided high-resolution observations of the Cytherean atmosphere and black-drop evolution. Our liaison with UH's Mees Solar Observatory scientists provided magneto-optical imaging at calcium and potassium. Solar Dynamics Observatory's AIA and HMI, and the Solar Optical Telescope (SOT) and X-ray Telescope (XRT) on Hinode, and total-solar-irradiance measurements with ACRIMSAT and SORCE/TIM, were used to observe the event as an exoplanet-transit analog. On September 20, we imaged Jupiter for 14 Hubble Space Telescope orbits, centered on a 10-hour ToV visible from Jupiter (J/ToV), as an exoplanet-transit analog in our own solar system, using Jupiter as an integrating sphere. Imaging was good, although much work remains to determine if we can detect the expected 0.01% solar irradiance decrease at Jupiter and the even slighter differential effect between our violet and near-infrared filters caused by Venus's atmosphere. We also give a first report on our currently planned December 21 Cassini UVIS observations of a transit of Venus from Saturn (S/ToV). Our E/ToV expedition was sponsored by the Committee for Research and Exploration/National Geographic Society; supplemented: NASA/AAS's Small Research Grant Program. We thank Rob Ratkowski, Stan Truitt, Rob Lucas, Aram Friedman, and Eric Pilger '82 at Haleakala, and Joseph Gangestad '06 at Big Bear for assistance, and Lockheed Martin Solar and Astrophysics Lab and Hinode science and operations teams for support for coordinated observations with NASA satellites. Our J/ToV observations were based on observations made with HST, operated by AURA, Inc., under NASA contract NAS 5-26555; these observations are associated with program #13067. Title: The 2012 Transit of Venus for Cytherean Atmospheric Studies and as an Exoplanet Analog Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Reardon, K. P.; Widemann, T.; Tanga, P.; Dantowitz, R.; Willson, R.; Kopp, G.; Yurchyshyn, V.; Sterling, A.; Scherrer, P.; Schou, J.; Golub, L.; Reeves, K. Bibcode: 2012DPS....4450806P Altcode: We worked to assemble as complete a dataset as possible for the Cytherean atmosphere in collaboration with Venus Express in situ and to provide an analog of spectral and total irradiance exoplanet measurements. From Haleakala, the whole transit was visible in coronal skies; our B images showed the evolution of the visibility of Venus's atmosphere and of the black-drop effect, as part of the Venus Twilight Experiment's 9 coronagraphs distributed worldwide with BVRI. We imaged the Cytherean atmosphere over two minutes before first contact, with subarcsecond resolution, with the coronagraph and a separate refractor. The IBIS imaging spectrometer at Sacramento Peak Observatory at H-alpha and carbon-dioxide also provided us high-resolution imaging. The NST of Big Bear Solar Observatory also provided high-resolution vacuum observations of the Cytherean atmosphere and black drop evolution. Our liaison with UH's Mees Solar Observatory scientists provided magneto-optical imaging at calcium and potassium. Spaceborne observations included the Solar Dynamics Observatory's AIA and HMI, and the Solar Optical Telescope (SOT) and X-ray Telescope (XRT) on Hinode, and total-solar-irradiance measurements with ACRIMSAT and SORCE/TIM, to characterize the event as an exoplanet-transit analog. Our expedition was sponsored by the Committee for Research and Exploration/National Geographic Society. Some of the funds for the carbon-dioxide filter for IBIS were provided by NASA through AAS's Small Research Grant Program. We thank Rob Lucas, Aram Friedman, and Eric Pilger '82 for assistance with Haleakala observing, Rob Ratkowski of Haleakala Amateur Astronomers for assistance with equipment and with the site, Stan Truitt for the loan of his Paramount ME, and Steve Bisque/Software Bisque for TheSky X controller. We thank Joseph Gangestad '06 of Aerospace Corp., a veteran of our 2004 expedition, for assistance at Big Bear. We thank the Lockheed Martin Solar and Astrophysics Laboratory and Hinode science and operations teams for planning and support. Title: The Solar Cycle 23 - 24 Minimum. A Benchmark in Solar Variability and Effects in the Heliosphere Authors: White, O.; Kopp, G.; Snow, M.; Tapping, K. Bibcode: 2011SoPh..274..159W Altcode: Given the numerous ground-based and space-based experiments producing the database for the Cycle 23 - 24 Minimum epoch from September 2008 to May 2009, we have an extraordinary opportunity to understand its effects throughout the heliosphere. We use solar radiative output in this period to obtain minimum values for three measures of the Sun's radiative output: the total solar irradiance, the Mg II index, and the 10.7 cm solar radio flux. The derived values are included in the research summaries as a means to exchange ideas and data for this long minimum in solar activity. Title: PREMOS Absolute Radiometer Calibration and Implications to on-orbit Measurements of the Total Solar Irradiance Authors: Fehlmann, A.; Kopp, G.; Schmutz, W. K.; Winkler, R.; Finsterle, W.; Fox, N. Bibcode: 2011AGUFMGC21C..05F Altcode: On orbit measurements starting in the late 1970's, have revealed the 11 year cycle of the Total Solar Irradiance (TSI). However, the absolute results from individual experiments differ although all instrument teams claim to measure an absolute value. Especially the data from the TIM/SORCE experiment confused the community as it measures 0.3 % lower than the other instruments, e.g. VIRGO/SOHO by PMOD/WRC, which clearly exceeds the uncertainty stated for the absolute characterization of the experiments. The PREMOS package on the PICARD platform launched in June 2010 is the latest space experiment by PMOD/WRC measuring the TSI. We have put great effort in the calibration and characterization of this instrument in order to resolve the inter-instrument differences. We performed calibrations at the National Physical Laboratory (NPL) in London and the Laboratory for Atmospheric and Space Physics (LASP) in Boulder against national SI standards for radiant power using a laser beam with a diameter being smaller than the aperture of the instrument. These measurements together with the World Radiometric Reference (WRR) calibration in Davos allowed to compare the WRR and the SI radiant power scale. We found that the WRR lies 0.18 % above the SI radiant power scale which explains a part of the VIRGO-TIM difference. The Total solar irradiance Radiometer Facility (TRF) at the LASP allows to generate a beam that over fills the apertures of our instruments, giving the presently best available representation of solar irradiance in a laboratory. These irradiance calibrations revealed a stray light contribution between 0.09 and 0.3 % to the measurements which had been underestimated in the characterization of our instruments. Using the irradiance calibrations, we found that the WRR lies 0.32 % above the TRF scale which in turn explains the full VIRGO-TIM difference. The first light PREMOS measurements in space confirmed our findings. If we use the WRR calibration, PREMOS yields a TSI value of 1365.5 ± 1.2 W/m2 (k=1) which is in excellent agreement with VIRGO (1365.4 W/m2). Else, applying the TRF calibration to PREMOS, we obtain a TSI value of 1360.9 ± 0.4 W/m2 (k=1) which is in excellent agreement with TIM (1361.3 W/m2). Title: Characterization of the DARA solar absolute radiometer Authors: Finsterle, W.; Suter, M.; Fehlmann, A.; Kopp, G. Bibcode: 2011AGUFMGC21C..07F Altcode: The Davos Absolute Radiometer (DARA) prototype is an Electrical Substitution Radiometer (ESR) which has been developed as a successor of the PMO6 type on future space missions and ground based TSI measurements. The DARA implements an improved thermal design of the cavity detector and heat sink assembly to minimize air-vacuum differences and to maximize thermal symmetry of measuring and compensating cavity. The DARA also employs an inverted viewing geometry to reduce internal stray light. We will report on the characterization and calibration experiments which were carried out at PMOD/WRC and LASP (TRF). Title: An Improved Total Solar Irradiance Climate Data Record Authors: Kopp, G. Bibcode: 2011AGUFMGC21C..03K Altcode: The dominant driver of the Earth's climate system is the Sun, which exceeds all other energy sources combined by a factor of 2500. Small as they are, variations in the enormous amount of energy received from the Sun can have climatic effects on the Earth over annual to millennial time scales. Climate studies rely on recent spaceborne measurements of total solar irradiance (TSI) and estimates of its historical variability to discern natural from anthropogenic climatic influences. Because the Sun is relatively stable, the TSI measurements providing this solar record must be of high accuracy, extremely good stability, and long duration. New instrument calibrations and diagnostics have improved the accuracy of the existing record and future instruments promise further improvements. I will discuss the status of the current solar climate data record based on recent findings, explain the climate-driven solar irradiance measurement requirements, show estimates of solar influences on climate, and give an overview of planned missions to provide this needed record for climate studies. Title: Infrared Cavity Radiometer Reflectometry in Support of Total Solar Irradiance Instruments Authors: Hanssen, L. M.; Zeng, J.; Wilthan, B.; Morrill, J. S.; Kopp, G. Bibcode: 2011AGUFMGC23A0911H Altcode: A key component required to achieve a high degree of accuracy in satellite solar irradiance measurements using cavity radiometers, is the characterization of the cavity spectral absorptance over the broad spectral range of the Solar output. This includes the infrared region up to at least 10 μm. In order to accurately measure high levels of absorptance of cavities, NIST has developed a laser and integrating sphere based facility (the Complete Hemispherical Infrared Laser-based Reflectometer (CHILR)). The system is used for both radiometer and blackbody cavity characterization. We report the results of reflectance (1 - absorptance) measurements of radiometer cavities designed for two solar irradiance measurement instruments: 1) the Active Cavity Radiometer Irradiance Monitor (ACRIM) and 2) the Total Irradiance Monitor (TIM) instrument on the SORCE and TSIS missions. The measurements were made using the NIST CHILR instrument as well as the Infrared Reference Integrating Sphere (IRIS) for relative spectral reflectance. The IRIS was used to obtain relative spectral reflectance for the TIM cones. The IRIS was also used to obtain the spectral reflectance of other surfaces in the ACRIM instrument that also interact with the incident irradiance and potentially affect the cavity performance. These reflectance results are used to validate previously estimated performance parameters of the two instruments. Title: A new, lower value of total solar irradiance: Evidence and climate significance Authors: Kopp, Greg; Lean, Judith L. Bibcode: 2011GeoRL..38.1706K Altcode: 2011GeoRL..3801706K The most accurate value of total solar irradiance during the 2008 solar minimum period is 1360.8 ± 0.5 W m-2 according to measurements from the Total Irradiance Monitor (TIM) on NASA's Solar Radiation and Climate Experiment (SORCE) and a series of new radiometric laboratory tests. This value is significantly lower than the canonical value of 1365.4 ± 1.3 W m-2 established in the 1990s, which energy balance calculations and climate models currently use. Scattered light is a primary cause of the higher irradiance values measured by the earlier generation of solar radiometers in which the precision aperture defining the measured solar beam is located behind a larger, view-limiting aperture. In the TIM, the opposite order of these apertures precludes this spurious signal by limiting the light entering the instrument. We assess the accuracy and stability of irradiance measurements made since 1978 and the implications of instrument uncertainties and instabilities for climate research in comparison with the new TIM data. TIM's lower solar irradiance value is not a change in the Sun's output, whose variations it detects with stability comparable or superior to prior measurements; instead, its significance is in advancing the capability of monitoring solar irradiance variations on climate-relevant time scales and in improving estimates of Earth energy balance, which the Sun initiates. Title: Fall 2010 Total Solar Irradiance Calibration Workshop Authors: Morrill, J. S.; Socker, D. G.; Willson, R. C.; Kopp, G. Bibcode: 2010AGUFMGC21B0870M Altcode: As part of a NASA-Sponsored program to understand the differences in Total Solar Irradiance (TSI) results reported by various space-based radiometers, the Naval Research Laboratory is hosting a Total Solar Irradiance Calibration Workshop. This workshop is a follow-on meeting to a similar workshop hosted by the National Institute for Standards and Technology in 2005. These workshops have been attended by many of the PI teams of the past and current TSI measuring instruments. The discussions at these workshops have addressed calibration methods and the numerous instrumental differences that need to be understood in order to bring the complete ensemble of results onto a common scale. In this talk we will present an overview of the NRL Calibration Workshop which will include results of recent calibration studies at various laboratories and have involved several TSI instruments. Title: Variability in SCIAMACHY Earth-Reflected Solar Spectral Radiance: Guidance for Climate Benchmarking Authors: Pilewskie, Peter; Roberts, Yolanda; Kindel, Bruce; Kopp, Greg Bibcode: 2010cosp...38...22P Altcode: 2010cosp.meet...22P The difference between the solar radiation incident at the top-of-the-atmosphere and that re-flected to space establishes the infrared emission required for radiative equilibrium and thus represents the most fundamental equation of climate. Detecting climate change signatures in reflected solar radiance has been hindered by instrument accuracy and stability, insufficient spectral coverage and resolution, and inherent sampling limitations from low-Earth orbit obser-vations. The primary goal of the Decadal Survey's Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission is to obtain climate "benchmark" data records with sufficient accuracy for identifying climate variability on decadal time scales and with sufficient informa-tion content to attribute change to underlying causality. Measurements of Earth-reflected solar spectral radiance from the ESA SCanning Imaging Absorption SpectroMeter for Atmospheric CHartographY (SCIAMACHY) have proven useful in defining a number of requirements for future missions that will establish climate benchmark data records. This paper presents results of CLARREO science definition studies utilizing the variability in SCIAMACHY spectra over spatial and temporal domains that can assist in defining the requirements of an Earth-viewing shortwave spectrometer for climate benchmarking. These same methods of analysis may also be applied to the detection of climate trends, and examples using SCIAMACHY spectra illustrate this capability. Title: Total solar irradiance record accuracy and recent improvements Authors: Kopp, Greg Bibcode: 2010cosp...38.1690K Altcode: 2010cosp.meet.1690K The total solar irradiance (TSI) data record includes uninterrupted measurements from over 10 spaceborne instruments spanning the last 31 years. Continuity of on-orbit measurements allows adjustments for instrument offsets to create a TSI composite needed for estimating solar influences on Earth's climate. Because climate sensitivities to solar forcings are determined not only from direct TSI measurements over recent 11-year solar cycles but also from reconstructions of historical solar variability based on the recent measurements, the accuracy of the TSI record is critical. This climate data record currently relies on both instrument stability and measurement continuity, although improvements in absolute accuracy via better instrument calibrations and new test facilities promise to reduce this current reliance on continuity. The Total Irradiance Monitor (TIM) is striving for improved levels of absolute accuracy, and a new TSI calibration facility is now able to validate the accuracy of modern instruments and diagnose causes of offsets between different TSI instruments. The instrument offsets are due to calibration errors. As of early 2010, none of the on-orbit instruments have been calibrated end-to-end to the needed accuracy levels. The new TSI Radiometer Facility (TRF) built for NASA's Glory mission provides these new calibration capabilities. Via direct optical power comparisons to a NIST-calibrated cryogenic radiometer, this ground-based facility provides calibrations of a TSI instrument much as the instrument is operated in space: under vacuum, at full solar irradiance power levels, and with uniform incoming light for irradiance measurements. Both the PICARD/PREMOS and the upcoming Glory/TIM instruments have been tested in this new facility, helping improve the absolute accuracy of the TSI data record and diagnose the causes of existing instrument offsets. In addition to being benchmarked to this new ground-based reference, the Glory/TIM and the future TSIS/TIMs are intended to achieve levels of absolute accuracy that should reduce the TSI record's reliance on measurement continuity. I will discuss the climate-derived requirements for the levels of absolute accuracy and instrument stability needed for TSI measurements and describe current work that is underway to achieve these measurement requirements. Title: Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle Authors: Domingo, V.; Ermolli, I.; Fox, P.; Fröhlich, C.; Haberreiter, M.; Krivova, N.; Kopp, G.; Schmutz, W.; Solanki, S. K.; Spruit, H. C.; Unruh, Y.; Vögler, A. Bibcode: 2009SSRv..145..337D Altcode: The uninterrupted measurement of the total solar irradiance during the last three solar cycles and an increasing amount of solar spectral irradiance measurements as well as solar imaging observations (magnetograms and photometric data) have stimulated the development of models attributing irradiance variations to solar surface magnetism. Here we review the current status of solar irradiance measurements and modelling efforts based on solar photospheric magnetic fields. Thereby we restrict ourselves to the study of solar variations from days to the solar cycle. Phenomenological models of the solar atmosphere in combination with imaging observations of solar electromagnetic radiation and measurements of the photospheric magnetic field have reached high enough quality to show that a large fraction (at least, about 80%) of the solar irradiance variability can be explained by the radiative effects of the magnetic activity present in the photosphere. Also, significant progress has been made with magnetohydrodynamic simulations of convection that allow us to relate the radiance of the photospheric magnetic structures to the observations. Title: The Solar Radiation and Climate Experiment (SORCE): Measuring the Sun's influence on climate from space Authors: Harder, J.; Snow, M.; Kopp, G.; Fontenla, J.; Pilewskie, P.; Richard, E.; Woods, T. Bibcode: 2009EGUGA..11.3317H Altcode: The NASA Solar Radiation and Climate Experiment, launched in January of 2003, is a suite of instruments that measures the variability of both the Sun's total solar irradiance (TSI) and its solar spectral irradiance (SSI) over the 110-2400 nm spectral range thereby accounting for more the 97% of the sun's radiant output. The SORCE spectrometers decompose the TSI signal into its spectral components, and the solar cycle trends in the 300-2400 nm have been measured for the first time. The SORCE instruments have revealed a number of important findings that have significance to the earth-climate system. 1) The Total Irradiance Monitor (TIM) measures the TSI with a precision of about1.0 part per million (ppm) and very small degradation that is correctable to about 10 ppm. Furthermore, recent laboratory studies support the absolute calibration of the instrument's reported Solar Cycle 23 solar minimum irradiance value of 1360.75 Wm-2, an important finding for Earth radiation budget analyses. 2) The time series from the Spectral Irradiance Monitor (SIM) shows that the observed TSI trends are the sum of offsetting spectral irradiance trends rather than the quasi-uniform change predicted from proxy/solar atmospheric models. These observed spectral irradiance changes will enable more realistic investigations of the mechanisms of climate responses to solar forcing. 3) The Solar Stellar Irradiance Comparison Experiment (SOLSTICE) is an ultraviolet spectrometer that was also onboard UARS satellite; the combined missions have a continuous observational record extending back to 1992 encompassing two solar minimum time periods. In the FUV portion of the spectrum (112-180 nm), the SOLSTICE data shows a lower spectral irradiance during the minimum of Solar Cycle 23 than during the minimum period of Solar Cycle 22 by about 5%. Title: SORCE Solar Irradiance Data Products Authors: Lindholm, D. M.; Pankratz, C. K.; Knapp, B. G.; Meisner, R.; Fontenla, J.; Harder, J. W.; McClintock, W. E.; Kopp, G.; Snow, M.; Woods, T. N. Bibcode: 2008AGUFMSM11B1623L Altcode: The Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado manages the SOlar Radiation and Climate Experiment (SORCE) Science Data System. This data processing system routinely produces Total Solar Irradiance (TSI) and Spectral Solar Irradiance (SSI) data products, which are formulated using measurements from the four primary instruments on board the SORCE spacecraft. The TIM instrument provides measurements of the TSI, whereas the SIM, SOLSTICE, and XPS instruments collectively provide measurements of the solar irradiance spectrum from 1 nm to 2400 nm (excluding 31-115 nm, which is measured by the SEE instrument on NASA's TIMED mission). Derived products, such as the Magnesium II Core-to-Wing Index which can be used for space weather applications, are also produced. The SORCE Science Data System utilizes raw spacecraft and instrument telemetry, calibration data, and other ancillary information to produce a variety of solar irradiance data products that have been corrected for all known instrumental and operational factors. Since launch of the SORCE spacecraft in January 2003, science processing algorithms have continued to mature, instrument calibrations (e.g. degradation corrections) have improved, and regularly updated versions of data products have been released. "Level 3" data products (time-averaged over daily and six-hourly periods and/or spectrally re-sampled onto uniform wavelength scales) are routinely produced and delivered to the public via the SORCE web site (http://lasp.colorado.edu/sorce/data/), and are archived at the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). Native resolution "Level 2" products are also available for scientific studies. This poster provides an overview of the SORCE data processing system, summarizes the present state of the processing algorithms, describes the quality of the current SORCE data products, provides details on how to access SORCE science data, and presents future plans. Title: TSIS: The Total Solar Irradiance Sensor Authors: Sparn, T.; Pilewskie, P.; Harder, J.; Kopp, G.; Richard, E.; Fontenla, J.; Woods, T. Bibcode: 2008AGUFM.A51F0165S Altcode: The Total Solar Irradiance Sensor (TSIS) is a dual-instrument package that will acquire solar irradiance in the next decade on the National Polar-orbiting Operational Environmental Satellite System (NPOESS). Originally de-manifested during the 2006 NPOESS restructuring, TSIS was restored following a decision by the NPOESS Executive Committee earlier this year because of its critical role in determining the natural forcings of the climate system and the high priority given it by the 2007 Earth Science Decadal Survey. TSIS is comprised of the Total Irradiance Monitor, or TIM, which measures the total solar irradiance (TSI) that is incident at the boundaries of the atmosphere; and the Spectral Irradiance Monitor, or SIM, which measures solar spectral irradiance (SSI) from 200 nm to 2400 nm (96 percent of the TSI). The TSIS TIM and SIM are heritage instruments to those currently flying on the NASA Solar Irradiance and Climate Experiment (SORCE). Both were selected as part of the TSIS because of their unprecedented measurement accuracy and stability, and because both measurements are essential to constraining the energy input to the climate system and interpreting the response of climate to external forcing. This paper will describe those attributes of TSIS which uniquely define its capability to continue the 30-year record of TSI and to extend the new 5-year record of SSI. The role of the solar irradiance data record in the present climate state, as well as in past and future climate change, will also be presented. Title: Spectral irradiance variations: comparison between observations and the SATIRE model on solar rotation time scales Authors: Unruh, Y. C.; Krivova, N. A.; Solanki, S. K.; Harder, J. W.; Kopp, G. Bibcode: 2008A&A...486..311U Altcode: 2008arXiv0802.4178U Aims: We test the reliability of the observed and calculated spectral irradiance variations between 200 and 1600 nm over a time span of three solar rotations in 2004.
Methods: We compare our model calculations to spectral irradiance observations taken with SORCE/SIM, SoHO/VIRGO, and UARS/SUSIM. The calculations assume LTE and are based on the SATIRE (Spectral And Total Irradiance REconstruction) model. We analyse the variability as a function of wavelength and present time series in a number of selected wavelength regions covering the UV to the NIR. We also show the facular and spot contributions to the total calculated variability.
Results: In most wavelength regions, the variability agrees well between all sets of observations and the model calculations. The model does particularly well between 400 and 1300 nm, but fails below 220 nm, as well as for some of the strong NUV lines. Our calculations clearly show the shift from faculae-dominated variability in the NUV to spot-dominated variability above approximately 400 nm. We also discuss some of the remaining problems, such as the low sensitivity of SUSIM and SORCE for wavelengths between approximately 310 and 350 nm, where currently the model calculations still provide the best estimates of solar variability. Title: Solar Spectral Irradiance Variability in the Near Infrared and Correlations to the Variability of Total Solar Irradiance During the Declining Phase of Solar Cycle 23 Authors: Richard, E. C.; Harder, J. W.; Fontenla, J.; Pilewskie, P.; Kopp, G.; Woods, T. N. Bibcode: 2007AGUFMGC31B0349R Altcode: The Spectral Irradiance Monitor (SIM) as part of the NASA EOS SORCE mission continuously monitors the solar spectral irradiance (SSI) across the wavelength region spanning the ultraviolet, visible and near infrared (a region encompassing >97% of the TSI measured by the SORCE Total Irradiance Monitor, TIM). These are the first daily measurements from space with the required precision to detect real changes in SSI. The record of TSI measured from space tracks changes in solar total energy output and establishes the baseline for energy input for the Earth. Where this radiative energy is deposited into the Earth system, how the climate responds to solar variability, and the mechanisms of climate response, are determined by how the incident solar radiation is distributed with wavelength, the SSI. For the near IR region in particular, spectral decomposition of the TSI variability provides TOA constraints on the direct input for atmospheric heating simulations. We present here the first long-term, continuous measurements of the near infrared variability of solar spectral irradiance and establish quantitative correlations of near infrared variability across the spectral region of the solar H minus opacity minimum with TSI variability. The unprecedented precision of the SIM near-infrared measurements provide a direct determination of the wavelength dependence of the facular and sunspot contrasts and serve to refine solar atmospheric models of the solar magnetic features that produce irradiance variability in emission from the deepest photospheric layers. Title: SORCE Solar Irradiance Data Products Authors: Lindholm, D. M.; Pankratz, C. K.; Knapp, B. G.; Meisner, R.; Fontenla, J.; Harder, J. W.; McClintock, W. E.; Kopp, G.; Snow, M.; Woods, T. N. Bibcode: 2007AGUFMSH13A1105L Altcode: The Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado manages the SOlar Radiation and Climate Experiment (SORCE) Science Data System. This data processing system routinely produces Total Solar Irradiance (TSI) and Spectral Solar Irradiance (SSI) data products, which are formulated using measurements from the four primary instruments on board the SORCE spacecraft. The TIM instrument provides measurements of the TSI, whereas the SIM, SOLSTICE, and XPS instruments collectively provide measurements of the solar irradiance spectrum from 1 nm to 2400 nm (excluding 31-115nm, which is measured by the SEE instrument on NASA's TIMED mission). The SORCE Science Data System utilizes raw spacecraft and instrument telemetry, calibration data, and other ancillary information to produce a variety of solar irradiance data products that have been corrected for all known instrumental and operational factors. Since launch of the SORCE spacecraft in January 2003, science processing algorithms have continued to mature, and "Level 3" data products (time-averaged and/or spectrally resampled onto uniform wavelength scales) are routinely being produced and delivered to the public via the SORCE web site, and are archived at the Goddard Earth Sciences (GES) Data and Information Services Center (DISC, formerly DAAC). This poster provides an overview of the SORCE data processing system, summarizes the present state of the processing algorithms and future plans, describes the quality of the current SORCE data products, and provides details on how to access SORCE science data. Title: Correlations Between Total Solar Irradiance and Spectral Irradiances Using SORCE Measurements Authors: Kopp, G. Bibcode: 2006AGUFMSH43A1504K Altcode: The SOlar Radiation and Climate Experiment (SORCE) was launched in January 2003 to measure both total solar irradiance (TSI) and spectral solar irradiance (SSI). The available spectral irradiances are contiguous from 115 nm to 1600 nm with nearly daily coverage, providing useful inputs to climate models since the Earth's atmospheric response is highly wavelength dependent. By correlating these relatively recent and short-duration spectral irradiances with simultaneous SORCE TSI measurements, the SSI may be linked to the nearly 3- decade long TSI record. Extending this SSI proxy via the TSI record may provide an estimate of historical spectral irradiances allowing comparisons to past climate. I present results from these wavelength-dependent correlations between SORCE TSI and SSI measurements. Title: Solar Irradiance Data for Space Weather from SORCE and TIMED-SEE Authors: Snow, M.; Woodraska, D.; McClintock, W. E.; Woods, T. N.; Kopp, G. Bibcode: 2006AGUFMSA53A1352S Altcode: The SOlar Radiation and Climate Experiment (SORCE) and Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) missions produce many solar irradiance data products of interest to the space weather community. The SOLar-STellar Irradiance Comparison Experiment (SOLSTICE) and Solar EUV Experiment (SEE) measure solar spectral irradiance below 300 nm, while the Total Irradiance Monitor (TIM) detects the Total Solar Irradiance. Ultraviolet and extreme ultraviolet solar spectral irradiances in defined bands are made available shortly after spacecraft contacts every day. Six-hour averages for the Magnesium II index and Total Solar Irradiance are also produced on a daily basis. These datasets are available via ftp for easy integration into the user's data stream. While these data come from research experiments rather than operational satellites, we have been able to make them reliably available for several years. The SOLSTICE Mg II index is often used as a redundant data source in case data from NOAA is unavailable. Additional space weather data products are planned from the Solar Dynamics Observatory (SDO) EUV Variability Experiement (EVE), which is scheduled for launch in August 2008. Title: Contributions of the solar ultraviolet irradiance to the total solar irradiance during large flares Authors: Woods, Thomas N.; Kopp, Greg; Chamberlin, Phillip C. Bibcode: 2006JGRA..11110S14W Altcode: The solar X-ray radiation varies more than other wavelengths during flares; thus solar X-ray irradiance measurements are relied upon for detecting flare events as well as used to study flare parameters. There is new information about the spectral and temporal variations of flares using solar irradiance measurements from NASA's Solar Radiation and Climate Experiment (SORCE) and the Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) missions. For one, the improved measurement precision for the total solar irradiance (TSI) measurements by the SORCE Total Irradiance Monitor (TIM) has enabled the first detection of flares in the TSI. These flare observations indicate a total flare energy that is about 105 times more than the X-ray measurements in the 0.1-0.8 nm range. In addition, solar spectral irradiance instruments aboard TIMED and SORCE have observed hundreds of flare events in the 0.1 nm to 190 nm range. These solar ultraviolet measurements show that the ultraviolet irradiance changes during flares account for 50% or more of the flare variations seen in the TSI, with most of the ultraviolet contribution coming from the ultraviolet shortward of 14 nm. The remaining part of the flare energy is assumed to come from the wavelengths longward of 190 nm, typically only needing to be about 100 ppm increase for the largest flares. Another result is that the flare variations in the TSI have a strong limb darkening effect, whereby the flares near the limb indicate variations in the TSI being almost entirely from the ultraviolet shortward of 14 nm. Title: SORCE Solar Irradiance Data Products Authors: Pankratz, C. K.; Knapp, B. G.; Fontenla, J. M.; Rottman, G. J.; Woods, T. N.; Harder, J. W.; Kopp, G.; McClintock, W. E.; Snow, M. Bibcode: 2005AGUFMSM43B1219P Altcode: The SORCE Science Data System produces Total Solar Irradiance (TSI) and Spectral Solar Irradiance (SSI) data products on a daily basis, which are formulated using measurements from the four primary instruments on board the SORCE spacecraft. The TIM instrument provides measurements of the TSI, whereas the SIM, SOLSTICE, and XPS instruments collectively provide measurements of the solar irradiance spectrum from 1 nm to 2700 nm (excluding 31-115 nm, which is measured by the TIMED SEE experiment). The Science Data System utilizes raw spacecraft and instrument telemetry, calibration data, and other ancillary information to produce a variety of data products that have been corrected for all known instrumental and operational factors. Since launch of the SORCE spacecraft in January 2003, science processing algorithms have continued to mature, and "Level 3" data products are routinely being produced and delivered to the public via the SORCE web site and the Goddard Earth Sciences (GES) Distributed Active Archive Center (DAAC). This poster provides an overview of the SORCE data processing system, summarizes the present state of the processing algorithms and future plans, describes the quality of the current SORCE data products, and provides details on how to access SORCE science data. The NPOESS TSIS instrument package will also include TIM and SIM instruments, having direct flight heritage from the SORCE mission, and will produce data products similar to those produced by the existing SORCE Science Data System. Title: The Absolute Accuracy of Space-Borne TSI Instruments: A Summary From the July 2005 TSI Accuracy Workshop Authors: Kopp, G.; Butler, J. J.; Lawrence, G. Bibcode: 2005AGUFMSH33C..05K Altcode: Space-borne measurements of the total solar irradiance (TSI) have been continuous since 1978 due to the temporal overlap from multiple instruments. Offsets between the several instruments contributing to the data record exceed the stated uncertainties of many of the instruments. To review the stated and assess the actual accuracies of the instruments, a workshop was held at NIST, Gaithersburg in July 2005 with speakers representing 7 of the space-borne TSI instruments. This workshop focused on two key areas of TSI measurement: 1) What is the absolute accuracy of each instrument? 2) How stable is each instrument, and thus how well can each track long-term changes in the TSI? We summarize the results of the workshop addressing the first of these questions, the absolute accuracy of the instruments. This is the 'Day 1' problem: after ground calibrations and launch, and prior to degradation from solar exposure and the space environment, how well does each instrument measure the true value of the TSI on an absolute scale? Title: The TSIS Sensors: Results and Instrument Analysis for the SORCE SIM Instrument Authors: Richard, E. C.; Harder, J. W.; Kopp, G.; Woods, T. N. Bibcode: 2005AGUFMSM51C..05R Altcode: The SORCE (SOlar Radiation and Climate Experiment) SIM (Spectral Irradiance Monitor) is a currently operating prism spectrometer that measures the solar spectrum four times a day in the 200-2700 nm region with a wavelength dependent resolution of 1 - 33 nm. SIM has been operational for 2.5 years and is now providing the first continuous record of solar variability throughout the visible and near infrared spectral regions and will continue this critical measurement on the upcoming TSIS mission. To fulfill the EDR (Environmental Data Record) for solar spectral irradiance, a number of in-flight instrument re-calibrations must be performed to account for possible instrument degradation processes that affect the pre-flight absolute calibration. This presentation will describe the in-flight recalibration steps currently used for SORCE and will be applied for TSIS, a summary of the planned preflight calibration, and present the SORCE spectral irradiance time series of solar spectral variability to demonstrate the need for these in-flight and pre-flight calibrations. Title: The TSIS Sensors: Current SORCE Results and Progress Toward NPOESS Authors: Kopp, G.; Rottman, G.; Harder, J.; Richard, E.; Viereck, R. Bibcode: 2005AGUFMSM51C..04K Altcode: The Total and Spectral Irradiance Sensor (TSIS) on the NPOESS is a combination of two solar irradiance instruments to monitor the solar energy incident at the top of the Earth's atmosphere. The first versions of these instruments are currently operating on NASA's SOlar Radiation and Climate Experiment (SORCE). The Total Irradiance Monitor (TIM) measures total solar irradiance (TSI) with high accuracy and precision, continuing a data record that has been uninterrupted since 1978. This TSI record is used both to determine solar forcing on the Earth's climate and to establish correlations with long duration proxies of solar activity, allowing estimates of past solar influences on the Earth. The Spectral Irradiance Monitor (SIM) measures the solar spectral irradiance from 0.2 to 2.7 microns. SIM data provide spectral resolution useful in determining the response of different layers in the Earth's atmosphere to solar variations and in diagnosing the solar causes of irradiance variations. A common pointing platform allows the two instruments to monitor the Sun almost continually without interfering with other NPOESS spacecraft operations. We present an overview of the TSIS requirements and sensors, status of the current SORCE measurements, progress on the NASA/Glory TIM (which continues the TSI data record from SORCE to TSIS), and current progress on TSIS. Title: Contributions of the Solar Ultraviolet Irradiance to the Total Solar Irradiance During Large Flares Authors: Woods, T. N.; Kopp, G. Bibcode: 2005AGUFMSA33A..07W Altcode: The TIMED satellite was launched in December 2001 and the SORCE satellite was launched in January 2003. Since then the solar activity has evolved from solar maximum conditions to moderately low activity in 2005. The XUV Photometer System (XPS), aboard both TIMED and SORCE, is measuring the solar soft X-ray (XUV) irradiance shortward of 34 nm with 7-10 nm spectral resolution and the bright hydrogen emission at 121.5 nm. The XPS instrument is best known for observing over 200 flares during the TIMED mission with its 3% solar observing duty cycle and over 800 flares during the SORCE mission with its 70% duty cycle. The XUV radiation, being mostly from coronal emissions, varies more than other wavelengths in the solar spectrum during a flare event, with each flare lasting from minutes to hours. The XPS measurements indicate variations by a factor of 50 for the largest flares during the October-November 2003 solar storm period and that the XUV variations can be as much as 20% of the total flare energy as determined from the total solar irradiance (TSI) measurements by the SORCE Total Irradiance Monitor (TIM). The flare variations of the solar XUV irradiance and TSI will be discussed in the context of the TIMED and SORCE missions and their relationship to the GOES X-ray flare measurements. Title: The spectral composition of TSI as measured by the SORCE SIM solar spectral radiometer Authors: Harder, J. W.; Fontenla, J.; Kopp, G.; Richard, E.; Woods, T. Bibcode: 2005AGUFMSH41A1113H Altcode: The SORCE (Solar Radiation and Climate Experiment) SIM (Spectral Irradiance Monitor) instrument is a satellite-borne prism spectrometer that measures the solar spectrum from 200-2700 nm with a cadence of at least 2 spectra per day and a wavelength dependent resolution of 1-33 nm. This instrument provides the temporal evolution of solar irradiance in the ultraviolet, visible, and infrared spectral regions. At some wavelengths in the ultraviolet, the SIM measurements exhibit variations similar to the Mg II core-to-wing ratio, and in the visible and IR they show similarities to the total solar irradiance (TSI) record, but with differing wavelength dependent amplitudes, phases, and shapes. Furthermore, the observed TSI variations can be examined in the context of the integral of the spectral irradiance over discrete spectral bands in the 200-1600 nm region showing the spectral contributions of solar active regions. Further insight into the solar variability observed by the SIM can be gained from analyzing the distribution of solar features as measured by the Precision Solar Photometric Telescope in conjunction with spectral decomposition (ApJ, 1999, 518, 480). Title: The Total Irradiance Monitor (TIM): Instrument Design Authors: Kopp, Greg; Lawrence, George Bibcode: 2005SoPh..230...91K Altcode: The Total Irradiance Monitor (TIM) instrument is designed to measure total solar irradiance with an absolute accuracy of 100 parts per million. Four electrical substitution radiometers behind precision apertures measure input radiant power while providing redundancy. Duty cycling the use of the radiometers tracks degradation of the nickel-phosphorous absorptive black radiometer interiors caused by solar exposure. Phase sensitive detection at the shutter frequency reduces noise and simplifies the estimate of the radiometer's equivalence ratio. An as-designed uncertainty budget estimates the instrument's accuracy goal. The TIM measurement equation defines the conversion from measured signal to solar irradiance. Title: The Total Irradiance Monitor (TIM): Instrument Calibration Authors: Kopp, Greg; Heuerman, Karl; Lawrence, George Bibcode: 2005SoPh..230..111K Altcode: The calibrations of the SORCE Total Irradiance Monitor (TIM) are detailed and compared against the designed uncertainty budget. Several primary calibrations were accomplished in the laboratory before launch, including the aperture area, applied radiometer power, and radiometer absorption efficiency. Other parameters are calibrated or tracked on orbit, including the electronic servo system gain, the radiometer sensitivity to background thermal emission, and the degradation of radiometer efficiency. The as-designed uncertainty budget is refined with knowledge from the on-orbit performance. Title: SORCE Contributions to New Understanding of Global Change and Solar Variability Authors: Lean, Judith; Rottman, Gary; Harder, Jerald; Kopp, Greg Bibcode: 2005SoPh..230...27L Altcode: An array of empirical evidence in the space era, and in the past, suggests that climate responds to solar activity. The response mechanisms are thought to be some combination of direct surface heating, indirect processes involving UV radiation and the stratosphere, and modulation of internal climate system oscillations. A quantitative physical description is, as yet, lacking to explain the empirical evidence in terms of the known magnitude of solar radiative output changes and of climate sensitivity to these changes. Reproducing solar-induced decadal climate change requires faster and larger responses than general circulation models allow. Nor is the indirect climatic impact of solar-induced stratospheric change adequately understood, in part because of uncertainties in the vertical coupling of the stratosphere and troposphere. Accounting for solar effects on pre-industrial surface temperatures requires larger irradiance variations than present in the contemporary database, but evidence for significant secular irradiance change is ambiguous. Essential for future progress are reliable, extended observations of the solar radiative output changes that produce climate forcing. Twenty-five years after the beginning of continuous monitoring of the Sun's total radiative output, the Solar Radiation and Climate Experiment (SORCE) commences a new generation of solar irradiance measurements with much expanded capabilities. Relative to historical solar observations SORCE monitors both total and spectral irradiance with significantly reduced uncertainty and increased repeatability, especially on long time scales. Spectral coverage expands beyond UV wavelengths to encompass the visible and near-IR regions that dominate the Sun's radiative output. The space-based irradiance record, augmented now with the spectrum of the changes, facilitates improved characterization of magnetic sources of irradiance variability, and the detection of additional mechanisms. This understanding provides a scientific basis for estimating past and future irradiance variations, needed for detecting and predicting climate change. Title: The Total Irradiance Monitor (TIM): Science Results Authors: Kopp, Greg; Lawrence, George; Rottman, Gary Bibcode: 2005SoPh..230..129K Altcode: The solar observations from the Total Irradiance Monitor (TIM) are discussed since the SOlar Radiation and Climate Experiment (SORCE) launch in January 2003. The TIM measurements clearly show the background disk-integrated solar oscillations of generally less than 50 parts per million (ppm) amplitude over the ∼2 ppm instrument noise level. The total solar irradiance (TSI) from the TIM is about 1361 W/m2, or 4-5 W/m2 lower than that measured by other current TSI instruments. This difference is not considered an instrument or calibration error. Comparisons with other instruments show excellent agreement of solar variability on a relative scale. The TIM observed the Sun during the extreme activity period extending from late October to early November 2003. During this period, the instrument recorded both the largest short-term decrease in the 25-year TSI record and also the first definitive detection of a solar flare in TSI, from which an integrated energy of roughly (6± 3)×1032 ergs from the 28 October 2003 X17 flare is estimated. The TIM has also recorded two planets transiting the Sun, although only the Venus transit on 8 June 2004 was definitive. Title: SORCE Solar Irradiance Data Products Authors: Pankratz, C. K.; Knapp, B. G.; Fontenla, J. M.; Rottman, G. J.; Woods, T. N.; Harder, J. W.; Kopp, G.; McClintock, W. E.; Snow, M. Bibcode: 2005AGUSMSH51B..03P Altcode: The SORCE Science Data System produces Total Solar Irradiance (TSI) and Spectral Solar Irradiance (SSI) data products on a daily basis, which are formulated using measurements from the four primary instruments on board the SORCE spacecraft. The TIM instrument provides measurements of the TSI, whereas the SIM, SOLSTICE, and XPS instruments collectively provide measurements of the solar irradiance spectrum from 1 nm to 3000 nm (excluding 31-115nm, which is covered by the TIMED SEE experiment). The Science Data System utilizes raw spacecraft and instrument telemetry, calibration data, and other ancillary information to produce a variety of data products that have been corrected for all known instrumental and operational factors. Since launch of the SORCE spacecraft in January 2003, science processing algorithms have continued to mature, and "Level 3" data products are routinely being produced and delivered to the public via the SORCE web site and the Goddard Earth Sciences (GES) Distributed Active Archive Center (DAAC). This poster provides an overview of the SORCE data processing system, summarizes the present state of the processing algorithms and the quality of the current SORCE data products, and provides details on how to access SORCE science data. Title: A Comparison of Total Solar Irradiance to the Mg II Index Based on SORCE Measurements Authors: Kopp, G.; Snow, M.; McClintock, W.; Woods, T. Bibcode: 2005AGUSMSH23B..04K Altcode: The reconstruction of the total solar irradiance (TSI) over the long-term often uses sunspot area and a faculae proxy such as the Mg II core-to-wing index (Mg index). With interest in validating this approach, we compare the Mg index to TSI measurements using data from NASA's SOlar Radiation and Climate Experiment (SORCE). The SORCE carries four solar irradiance instruments that have been monitoring the Sun since early 2003. The Total Irradiance Monitor (TIM) measures the TSI with unprecedented stability and low noise during the daytime portion of each spacecraft orbit with a time cadence of 100 seconds. The SOLar STellar Irradiance Comparison Experiment (SOLSTICE) measures solar spectral irradiance from 115 to 320 nm, having 0.1 nm spectral resolution at the Mg II lines near 280 nm. The Mg II lines are scanned approximately seven times each day, and the Mg index provides a good indicator of chromospheric activity. We compare the SOLSTICE Mg II core-to-wing index to TIM TSI measurements, giving advantages over previous comparisons including simultaneity, low noise, and high spectral resolution for the Mg II lines. Title: TIM Degradation Rates and Possibilities of Measuring Secular TSI Changes Authors: Kopp, G.; Lawrence, G.; Rottman, G. Bibcode: 2004AGUFMSH53A0302K Altcode: We present the on-orbit degradation measured on the Total Irradiance Monitor (TIM), a total solar irradiance (TSI) monitoring instrument on NASA's SOlar Radiation and Climate Experiment (SORCE). The monitored degradation to date is extremely small (50 ppm/yr) with an uncertainty of 10 ppm/yr. We discuss the possibilities of accurately measuring secular changes in TSI using instruments with comparable degradation rates. Title: GOMOS Ozone Profile Validation Using Data From Ground-Based and Balloon-Sonde Measurements Authors: Meijer, Y. J.; Swart, D. P. J.; Allaart, M.; Andersen, S. B.; Bodeker, G.; Boyd, I.; Braathen, G.; Calisesi, Y.; Claude, H.; Dorokhov, V.; von der Gathen, P.; Gil, M.; Godin-Beekmann, S.; Goutail, F.; Hansen, G.; Karpetchko, A.; Keckhut, P.; Kelder, H. M.; Koelemeijer, R.; Kois, B.; Koopman, R. M.; Lambert, J. -C.; Leblanc, T.; McDermid, I. S.; Pal, S.; Kopp, G.; Schets, H.; Stübi, R.; Suortti, T.; Visconti, G.; Yela, M. Bibcode: 2004ESASP.562E..61M Altcode: 2004acve.conf...61M One of the nine instruments on-board the polar-orbiting environmental satellite ENVISAT is the Global Ozone Monitoring by Occultation of Stars (GOMOS) instrument. This paper presents validation results of GOMOS ozone profiles (v6.0a) from comparisons to microwave radiometer, balloon ozonesonde and lidar measurements worldwide. Thirty-one instruments/ launch-sites at twenty-five stations ranging from the Arctic to the Antarctic joined in this activity. We identified 3,713 useful collocated observations that were performed within an 800-km radius and a maximum 20hours time difference of a satellite observation, for the period June 2002 and March 2003. These collocated profiles were compared and the results were analyzed for possible dependencies on several geophysical (e.g., latitude) and GOMOS observational (e.g., star characteristics) parameters. In a dark atmospheric limb the GOMOS data agree very well with the correlative data and between 20- to 61-km altitude their differences only show a small (2.5%) insignificant negative bias with a standard deviation of about 14%. This conclusion is demonstrated to be independent of the star temperature and magnitude, and the latitudinal region of the GOMOS observation Title: Validation of SCIAMACHY Ozone Column Densities and Profiles Using Ground-Based FTIR and Millimeter Wave Measurements Authors: Kopp, G.; Blumenstock, Th.; Brinksma, E.; Eskes, H.; Griesfeller, A.; Hase, F.; Hochschild, G.; Kramer, I.; Mikuteit, S.; Raffalski, U.; van der A, R. Bibcode: 2004ESASP.562E..35K Altcode: 2004acve.conf...35K Ground-based FTIR and millimeter wave measurements of the Institute of Meteorology and Climate Research (IMK), Forschungszentrum Karlsruhe, and the Swedish Institute of Space Physics (IRF) are used for validation of SCIAMACHY ozone measurements. FTIR and millimeter wave measurements used for this study were routinely carried out between 2002 and 2004 at IRF at Kiruna, Sweden. In addition IMK carried out millimeter wave measurements on Mount Zugspitze in the Alps in 2003. SCIAMACHY level 2 NRT-products of 2002 are only validated by FTIR data since millimeter wave observations started in late 2002 when SCIAMACHY data were unavailable. For the years 2003 and early 2004 total ozone column abundances retrieved with the TOSOMI algorithm of the Royal Netherlands Meteorological Institute (Koninklijk Nederlands Meteorologisch Instituut, KNMI) are validated by the FTIR and microwave measurements. Finally, ozone limb profiles between July and November 2002 taken from the current SCIA Level 2 Off-Line masterset are validated by the FTIR measurements at Kiruna Title: SCIMACHY Ozone Profile Validation Authors: Brinksma, E. J.; Piters, A. J. M.; Boyd, L. S.; Parrish, A.; Bracher, A.; von Savigny, C.; Bramstedt, K.; Schmoltner, A. -M.; Taha, G.; Hilsenrath, E.; Blumenstock, T.; Kopp, G.; Mikuteit, S.; Fix, A.; Meijer, Y. J.; Swart, D. P. J.; Bodeker, G. E.; McDermid, I. S.; Leblanc, T. Bibcode: 2004ESASP.562E..15B Altcode: 2004acve.conf...15B No abstract at ADS Title: Validation of MIPAS and SCIAMACHY Data by Ground-Based Spectroscopy at Kiruna, Sweden, and Izana, Tenerife Island (AOID-191) Authors: Blumenstock, T.; Mikuteit, S.; Griesfeller, A.; Hase, F.; Kopp, G.; Kramer, I.; Schneider, M.; Fischer, H.; Gil, M.; Moreta, J. R.; Navarro Coma, M.; Raffalski, U.; Cuevas, E.; Dix, B.; Schwarz, G. Bibcode: 2004ESASP.562E..49B Altcode: 2004acve.conf...49B Within this ENVISAT validation project [AOID-191] ground-based measurements of different techniques have been performed at Kiruna in the Arctic and on Tenerife Island in the subtropics. These ground-based data were used to validate SCIAMACHY and MIPAS data. Using MIPAS 4.61 O3 profiles on a pressure scale and degrading their vertical resolution to that of the FTIR profiles a good agreement is demonstrated. The precision of FTIR O3 profiles is about 10 %. The differences between MIPAS and FTIR are within the combined error bar. MIPAS 4.61 HNO3 profiles differ about 10 to 15 % for altitudes above 15 km. The corresponding column amounts differ by 8.2 +/- 7.0 %. These differences can be explained by a scaling factor in the spectroscopic data base for HNO3 which has been applied in version 4.61. SCIAMACHY O3 and NO2 column amounts of versions 5.01 agree much better as compared to previous versions: The difference of SCIAMACHY O3 column amounts is about 8 % when compared to FTIR data from Kiruna and about 2 % when compared with DOAS data from Izaña, respectively. The difference of SCIAMACHY NO2 column amounts to Izaña DOAS data is about 9 %. Furthermore, O3 limb profiles from SCIAMACHY have been compared for the first time. The mean differences are up to 20%. However, shifting the SCIAMACHY profiles by +1.5 km reduces the discrepancies significantly. Then the mean relative difference is smaller than 10% for all altitude levels between 10 and 35 km. This shift is consistent with the erroneous height assignment of MIPAS profiles Title: Solar irradiance variability during the October 2003 solar storm period Authors: Woods, Thomas N.; Eparvier, Francis G.; Fontenla, Juan; Harder, Jerald; Kopp, Greg; McClintock, William E.; Rottman, Gary; Smiley, Byron; Snow, Martin Bibcode: 2004GeoRL..3110802W Altcode: The extraordinary solar storms between 18 October 2003 and 5 November 2003 include over 140 flares, primarily from two different large sunspot groups. There were 11 large X-class flares during this period, including an X17 flare on 28 October 2003 and an X28 flare on 4 November 2003. The X28 flare is the largest flare since GOES began its solar X-ray measurements in 1976. The solar (full-disk) irradiance during these flares was observed by the instruments aboard the NASA Solar Radiation and Climate Experiment (SORCE) spacecraft and the NASA Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) spacecraft. The total solar irradiance (TSI) dropped by unprecedented 0.34% during this period due to the dark, large sunspots. In addition, the TSI increased by 270 ppm during the X17 (4B optical) flare on 28 October, the first definitive measurement of a TSI flare event. The ultraviolet (UV) variations for this X17 flare range from a factor of about 50 shortward of 10 nm to about 10% for the Mg II 280 nm emission. One interesting result for the UV flare variations is that the broad wings of the H I Lyman-α (121.6 nm) emission increased by more than a factor of 2 during the X17 flare while the core of the Lyman-α emission only increased by 20%. Another interesting result is the time profile of the Si III 120.6 nm emission, which shows a sharp 1-minute long increase by a factor of 17 during the impulsive phase. Title: Total Solar Irradiance Observations of the Oct./Nov. 2003 Solar Flares Authors: Kopp, G.; Lawrence, G. M.; Rottman, G.; Woods, T. Bibcode: 2004AAS...204.0215K Altcode: 2004BAAS...36..669K We report on the first definitive observation of a solar flare in total solar irradiance (TSI) and on TSI observations of several other flares during the active Oct./Nov. time period. Solar flares are most prominent in EUV or X-ray wavelengths, since they release significant energy in these spectral regions where the Sun itself has a relatively low background. Despite their high energies, flares are minuscule compared to the entire energy output of the Sun, and thus cause very little change in TSI. Indeed, in 25 years of space-based irradiance monitoring prior to October 2003, no previous solar flare had been measured in TSI.

The Oct. 28, 2003 X17 flare was measured by the Total Irradiance Monitor (TIM) on NASA's SORCE. The TIM measures power across the entire solar spectrum, integrating X-ray to far infrared wavelengths. TIM data show a sudden increase of almost 270 parts per million slightly preceding the flare's soft X-ray peak at 11:10 UT. The TSI signature is similar to hard X-ray emissions in that it roughly coincides with the maximum rate of change of the soft X-ray emission.

The TSI measurement provides the spectrally integrated flare energy. We estimate the Oct. 28 flare had total energy exceeding 4.6e25 Joules. Preliminary estimates of the flare energy at wavelengths shorter than 200 nm, based on solar EUV measurements from other SORCE instruments and from an instrument on NASA's TIMED mission, only account for 23% of this energy, meaning the majority of the flare's energy was at longer wavelengths. This, combined with the timing of the flare in TSI, may indicate that portions of the visible and UV included in TSI also respond to the initiation phase of the flare.

We appreciate the support of NASA for this work. Title: Remarkable Low Temperature Emission of the 4 November 2003 Limb Flare Authors: Leibacher, J. W.; Harvey, J. W.; Kopp, G.; Hudson, H.; GONG Team Bibcode: 2004AAS...204.0213L Altcode: 2004BAAS...36..669L Strong (> 1.5 times normal intensity) continuum and photospheric line emission of the 4 November 2003 X28 flare was recorded simultaneously by three widely separated GONG instruments. Emission was seen from on the disk to > 20" above the limb for nearly one hour, likely making this event the longest duration white light flare observed to date. GONG observations are one-minute duration integrations of intensity averaged across a Lyot filter bandpass of about 90 pm FWHM centered on the Ni I line at 676.8 nm with 2.5" instrument pixel size. Spatial resolution is limited by diffraction and seeing to greater than 5". Additional measurements include the Doppler shift and strength of the spectrum line. These latter measurements indicate that continuum and line emission contributed about equally to the observed intensity signal. Light curves and images of the flare show a notable two-kernel disk event starting at about 19:33 UTC followed by a much stronger event that peaked at about 19:44. Rare, white-light prominences were visible above the limb after 19:34. Comparison of total solar irradiance measurements from the TIM instrument on board the SORCE spacecraft with full-disk integrated GONG intensities shows the global five-minute oscillation and the white light flare. The latter is much weaker in the GONG data, suggesting that most of the TIM flare signal arises from other, most likely shorter, wavelengths.

This work utilizes data obtained by the Global Oscillation Network Group (GONG) Program, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. SORCE is supported by NASA NAS5-97045 Title: Irradiance Observations of the October 28, 2003 X-17 Flare Authors: Rottman, G.; Woods, T.; Kopp, G.; McClintock, W.; Snow, M.; Fontenla, J.; Harder, J. Bibcode: 2004AGUSMSH31B..02R Altcode: The Solar Radiation and Climate Experiment, SORCE, carries four instruments that measure solar irradiance -- both total solar irradiance, TSI, and spectral irradiance from soft X-rays, ultraviolet, visible and near infrared. During the X-17 flare at 11:00 UT on October 28, 2003 the SORCE instruments were in ideal configurations to record increases in TSI and at most observed wavelengths. The X-ray and UV irradiance originating in the transition region and corona increased by factors as large as fifty. This large flare also provided the first measurement of an increase in TSI, a unique measurement that places an important new constraint on the energy release during the flare. This report is a survey and interpretation of the irradiance variations observed during this X-17 flare. Title: Total irradiance monitor design and on-orbit functionality Authors: Kopp, Greg; Lawrence, George; Rottman, Gary Bibcode: 2004SPIE.5171...14K Altcode: The solar Total Irradiance Monitor (TIM) on NASA's SORCE mission began taking data in early 2003. This instrument continues the 25-year record of space-borne, total solar irradiance (TSI) measurements, with improved precision from its new technologies and calibration methods. We present an overview of the TIM instrument, including the design features enabling its high precision, and we present preliminary on-orbit TSI data. Title: What is the Accuracy of the Total Irradiance Monitor? Authors: Kopp, G. A.; Lawrence, G.; Rottman, G. Bibcode: 2003AGUFMSH31C..07K Altcode: The Total Irradiance Monitor (TIM) on NASA's SOlar Radiation and Climate Experiment (SORCE) is the most recently launched instrument to monitor the total solar irradiance (TSI). We present results from the first of the TIM's five years of operations and discuss the current knowledge of the instrument's accuracy. To date, we find the four instrument channels in good agreement and extremely robust against solar exposure. Such instrument characterizations and measurement accuracies influence the observational scenarios appropriate for determining long-term solar variability, and currently favor overlapping measurements of very stable TSI-monitoring instruments. Title: Liquid crystal intensity modulator for simulating planetary transits Authors: Kopp, Greg Bibcode: 2003SPIE.5170..229K Altcode: I describe a liquid crystal intensity modulator designed to achieve <10 parts per million (ppm) modulation to simulate a planetary transit like those required for ground testing of NASA's Kepler mission. The design uses a nematic liquid crystal as a variable retarder aligned between two linear polarizers, with the retardance values and the alignment chosen to provide low sensitivity of transmitted intensity to input liquid crystal voltage variations. Modulator test results give intensity fluctuations of a few ppm from millivolt modulations about the input 8 V baseline voltage. Title: Phase Sensitive Detection for the SORCE Total Irradiance Monitor Authors: Kopp, G.; Lawrence, G.; Rottman, G.; Woods, T. Bibcode: 2002AGUFMSH52A0496K Altcode: The Total Irradiance Monitor (TIM) on the SOlar Radiation and Climate Experiment (SORCE) will measure the total solar irradiance (TSI). The TIM will report four TSI measurements daily, continuing the current 24-year record of solar irradiance through SORCE's goal 5-year mission life. This instrument was designed to achieve a relative standard uncertainty (1 σ precision) of 100 parts per million (ppm) and a precision and long-term uncertainty of 10 ppm/year. The major innovation the TIM brings to spaceborne TSI measurements is phase sensitive detection. This new instrument was designed from the ground up with the primary consideration being low-noise performance at the shutter fundamental, minimizing parasitic effects at and in-phase with the instrument's shutter. The DSP-controlled thermal balance and this phase sensitive detection method reduce sensitivity to thermal fluctuations and noise, enabling the instrument's high precision. We describe in detail here the phase sensitive detection algorithm used for the TIM. Title: A summary of spacecraft measurements of total solar irradiance Authors: Kopp, G.; Lawrence, G.; Rottman, G. Bibcode: 2002cosp...34E.694K Altcode: 2002cosp.meetE.694K The mean total solar irradiance (TSI) varies about 0.1% over a solar cycle, with 0.3% variability on time scales of a few weeks due to active regions on the Sun. Accurate measurements of TSI from above the Earth's atmosphere have been contiguous since 1978. Each of the dozen instruments contributing a TSI time series to this data set shows high sensitivity, detecting small changes in the Sun's relative output. Absolute accuracy is less precise, giving offsets between the instruments that are in some cases greater than the level of solar variability. Long-term trends in the solar irradiance are difficult to determine but tantalizingly close with the instruments' measurement accuracies and with the two solar cycles of measurements now available. We will summarize the spaceborne TSI measurements and the results obtained from these several missions. We discuss the relative and absolute instrument accuracies, leading to the observing time lengths needed for detecting trends in the solar irradiance. We will mention future missions that will continue the TSI data set and discuss their expected accuracies. Title: SORCE - Continuing Measurements of Solar Irradiance Authors: Kopp, G.; Rottman, G.; Woods, T.; Harder, J.; Lawrence, G.; McClintock, B.; Adda, M. Bibcode: 2001AGUFM.A51E0085K Altcode: The NASA/EOS Solar Radiation and Climate Experiment (SORCE) will measure the total and the spectral irradiance from the Sun, continuing the solar data record from the Upper Atmosphere Research Satellite (UARS). Four SORCE instruments provide irradiance measurements at wavelengths from 1 nm to longer than 2000 nm. The Total Irradiance Monitor (TIM) measures total solar irradiance (TSI), similar to the UARS/ACRIM instrument. The TIM will achieve a relative standard uncertainty (1 σ precision) of 100 parts per million (ppm), continuing the 23-year record of TSI measurements. SORCE's two SOLar STellar Irradiance Comparison Experiment (SOLSTICE) instruments are nearly identical to the SOLSTICE flown on UARS. These grating spectrometers monitor the more highly-variable solar ultraviolet irradiance over the wavelength range 120 to 300 nm with a 2 to 5% absolute uncertainty and a capability of making relative solar variability measurements with an accuracy of 0.5% by using stable, blue stars for in-flight calibration. The Spectral Irradiance Monitor (SIM) is a new prism spectrometer providing the first continuous solar spectral irradiance measurements from 200 to 2000 nm with 300 ppm uncertainty. The XUV Photometer System (XPS) covers 1 to 35 nm using 9 spectral bandpass filters to measure the large solar irradiance variations in the extreme ultraviolet with a ~20% accuracy. Launching in July of 2002 with a mission life goal of 5 years, SORCE will extend the UARS solar irradiance database in time as well as spectral region. SORCE data will be available via NASA/GSFC's Distributed Active Archive Center (DAAC) as well as from LASP's web site (http://lasp.colorado.edu/sorce). Title: SORCE - The Solar Radiation and Climate Experiment Authors: Kopp, G.; Rottman, G.; Harder, J.; Lawrence, G.; McClintock, B.; Woods, T. Bibcode: 2001AGUSM..SH52A08K Altcode: The NASA/EOS Solar Radiation and Climate Experiment (SORCE) will measure the total and the spectral irradiance from the Sun, providing inputs for understanding the Earth's climate. Four instruments provide irradiance measurements at wavelengths from 1 nm to longer than 2000 nm as follows: The Total Irradiance Monitor (TIM) measures total solar irradiance (TSI) to a relative standard uncertainty (1 σ precision) of 100 parts per million (ppm). The TIM will continue the current 22-year record of solar irradiance measurements using a modern phase-sensitive electronics design. The Spectral Irradiance Monitor (SIM) provides the first continuous spectral irradiance measurements from 200 to 2000 nm. This prism spectrometer will achieve 300 ppm uncertainty and a spectral resolution ranging from 0.2 to 30 nm. The Solar Stellar Irradiance Comparison Experiment (SOLSTICE) monitors the more highly-variable solar ultraviolet irradiance with a ~5% uncertainty over the wavelength range 120 to 300 nm. This grating spectrometer has 0.1 to 0.2 nm spectral resolution, and uses measurements of stable, blue stars for in-flight calibration. This SORCE instrument continues the data record from the Upper Atmospheric Research Satellite's SOLSTICE. The XUV Photometer System (XPS) covers 1 to 35 nm using 9 spectral bandpass filters to measure the large solar irradiance variations in the extreme ultraviolet with a ~20% accuracy. A nearly identical instrument launches on the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) mission in August 2001. SORCE will be launched on a Pegasus XL into a low Earth orbit in July of 2002 with a mission life goal of 5 years. Total and spectral irradiance data will be available via NASA/GSFC's Distributed Active Archive Center (DAAC) as well as from LASP's web site (http://lasp.colorado.edu/sorce). Title: Optical design for Terrestrial Planet Finder Authors: Noecker, M. C.; Leitch, James W.; Kopp, Greg A.; McComas, Brian K. Bibcode: 1999SPIE.3779...40N Altcode: We describe the features of the optical system for Terrestrial Planet Finder, a space-based, cryogenic interferometer for direct detection of Earth-type planets around nearby stars. Destructive interference in a stellar interferometer suppresses stellar glare by a factor of several thousand or more, and phase chopping distinguishes planet light from symmetric backgrounds. The mid-IR is favorable for detecting planetary emission relative to that from the star, and this spectral region also offers important molecular signatures indicative of key atmospheric gases. Title: The vertical distribution of ClO at Ny-Ålesund during March 1997 Authors: Ruhnke, R.; Kouker, W.; Reddmann, Th.; Berg, H.; Hochschild, G.; Kopp, G.; Krupa, R.; Kuntz, M. Bibcode: 1999GeoRL..26..839R Altcode: Results of the Karlsruhe Simulation Model of the Middle Atmosphere (KASIMA) are compared with vertical ClO profiles measured by the ground-based Millimeter Wave Radiometer MIRA2 inside the vortex during March 1997 at Ny-Ålesund. The influence of the OH + ClO and HO2 + ClO reaction branching ratio and of the absorption cross section of Cl2O2 on the calculated mixing ratios of ClO and ozone has been investigated. In the upper stratosphere the ClO mixing ratio is reduced by 90% by using a minor channel of the OH + ClO reaction with a branching ratio of 0.07. A temperature dependent minor channel of the HO2 + ClO reaction reduces the upper stratospheric ClO mixing ratio by 22%. Different absorption spectra of Cl2O2 alter the ClO mixing ratios up to 12% at noon at 20 km. This causes differences of 15% in the ozone loss during winter. Title: Optical design for Terrestrial Planet Finder. Authors: Noecker, M. C.; Kopp, G.; Leitch, J.; McComas, B. Bibcode: 1999aero....4...59N Altcode: The authors describe the features of the optical system for the Terrestrial Planet Finder, a space-based, cryogenic (35K) interferometer for direct detection of Earth-type planets around nearby stars. Interferometric nulling suppresses stellar glare by a factor of several thousand or more, and phase chopping distinguishes planet light from the symmetric background. The mid-infrared (7 - 20 μm) is favorable for detecting planetary emission relative to that from the star, and this spectral region also offers important molecular signatures indicative of key atmospheric gases. Title: Outline of an optical design for Terrestrial Planet Finder Authors: Noecker, Charley; McComas, Brian K.; Kopp, Greg A. Bibcode: 1998SPIE.3356..641N Altcode: A nulling interferometer for direct detection and spectral studies of the light from extra-solar planets would face daunting technical challenges. We outline a candidate optical architecture, discussing the major challenges in handling the starlight and controlling the optics to produce a deep on-axis null with high transmission a fraction of an arcsecond away. Title: Laser metrology for space interferometry Authors: Leitch, James W.; Kopp, Greg A.; Noecker, Charley Bibcode: 1998SPIE.3350..526L Altcode: Several proposed spacecraft missions require positional knowledge of their optical elements to very high precision. This knowledge can be provided by a metrology system based on a laser interferometer incorporating the spacecraft optics. We present results from fabrication and testing of a lab-based frequency-modulated (FM) Michelson interferometer intended to maintain length stability to a few picometers. The instrument can be used to make precise relative distance measurements or it can be used to characterize orientation and polarization effects of system components commonly used in metrology gauges. External frequency modulation of a frequency-stabilized laser source and phase-sensitive detection are used to detect changes in the arm length difference of the interferometer. Arm length adjustments are made via a closed loop feedback system. A second system having a shared beampath with the primary system monitors the performance of the primary system. Preliminary data, operating in an ambient lab environment, demonstrate control to roughly 20 picometers rms for measurement times around 100 seconds. Title: Subnanometer laser metrology for spacecraft interferometry Authors: Leitch, James W.; Kopp, Greg A.; Noecker, Charley Bibcode: 1998SPIE.3479...62L Altcode: Several proposed space-based interferometry missions require positional knowledge of their optical elements to very high precision. To achieve the desired stellar position measurement precision, the internal optical path difference of the stellar interferometer must be measured to within 10 picometers. This knowledge can be provided by a metrology system based on a laser interferometer incorporating the spacecraft optics. We present results from fabrication and testing of a lab-based frequency-modulated (FM) Michelson interferometer intended to maintain length stability to a few picometers. The instrument can be used to make precise relative distance measurements or it can be used to characterize orientation and polarization effects of system components commonly used in metrology gauges. External frequency modulation of a frequency- stabilized laser source and phase-sensitive detection are used to detect changes in the arm length difference of the interferometer. Arm length adjustments are made via a closed loop feedback system. A second system having a shared beampath with the primary system monitors the performance of the primary system. Preliminary data, operating in an ambient lab environment, demonstrate control to roughly 6 picometers rms for measurement times around 10 seconds. Title: Tunable liquid-crystal filter for solar imaging at the He i 1083-nm line Authors: Kopp, G. A.; Derks, M. J.; Elmore, D. F.; Hassler, D. M.; Woods, J. C.; Streete, J. L.; Blankner, J. G. Bibcode: 1997ApOpt..36..291K Altcode: No abstract at ADS Title: Submillimeter Radiometry of Sunspots Authors: Lindsey, C.; Kopp, G. Bibcode: 1995ApJ...453..517L Altcode: We use observations of sunspots by the 15 m James Clerk Maxwell Telescope (JCMT) for radiometry of sunspot umbrae and penumbrae The observations reported here, taking account of the effects of the far wings of the JCMT's beam, show that sunspot umbrae and penumbrae vary considerably in brightness between one another. The sunspot umbra is typically considerably dimmer than the quiet Sun but surrounded by a penumbra that may be fully as bright as surrounding plage. Moreover, the vertical brightness temperature gradients of sunspot umbrae and penumbrae appear to be uniformly positive, roughly equivalent to that of the quiet Sun. This gradient substantiates the operation of nonradiative heating in the low chromospheres of the strongest magnetic regions visible on the Sun's surface, i.e., sunspot umbrae. Title: The Sun in Submillimeter and Near-Millimeter Radiation Authors: Lindsey, C.; Kopp, G.; Clark, T. A.; Watt, G. Bibcode: 1995ApJ...453..511L Altcode: We examine the best solar submillimeter observations made on the James Clerk Maxwell Telescope in 1991 and 1992. In these observations, the solar disk was observed concurrently in pairs of wavelengths chosen from 350, 850, and 1200 μm. Images at all of these wavelengths show clear limb brightening of the quiet Sun. The observations clearly resolve the chromospheric supergranular network in active and quiet regions. The quiet Sun is characterized by large-scale variations in brightness, particularly the occasion of anomalously dark regions that tend to surround active regions. Sunspots are clearly resolved, with large dark umbrae clearly distinguished from sometimes particularly bright penumbrae. Title: Removing Instrumental Polarization from Infrared Solar Polarimetric Observations Authors: Kuhn, J. R.; Balasubramaniam, K. S.; Kopp, G.; Penn, M. J.; Dombard, A. J.; Lin, H. Bibcode: 1994SoPh..153..143K Altcode: Full Stokes polarimetry is obtained using the National Solar Observatory Vacuum Tower Telescope at Sacramento Peak while observing the magnetically sensitive infrared FeI line at wavelength of 1.56μ. A technique is described which makes use of the high magnetic resolution in this spectral range to remove instrumental polarization from observed StokesQ, U, andV line profiles. Title: A Magnetic Field Strength vs. Temperature Relation in Sunspots Authors: Kopp, G.; Rabin, D. Bibcode: 1994IAUS..154..477K Altcode: No abstract at ADS Title: Observations of seeing at 0.5 and 12.4 μm Authors: Livingston, W.; Kopp, G.; Gezari, D.; Varosi, F. Bibcode: 1994IAUS..158..299L Altcode: No abstract at ADS Title: Imaging Solar Bolometric and Spectral Intensity Using Thermal Detector Arrays Authors: Deming, D.; Glenar, D.; Kostiuk, T.; Bly, V.; Forrest, K.; Nadler, D.; Hudson, H.; Lindsey, C.; Kopp, G.; Avrett, E.; Terrill, C. W. Bibcode: 1993BAAS...25R1221D Altcode: No abstract at ADS Title: Sunspot and Active Region Chromospheres from Submillimeter JCMT Observations Authors: Kopp, G.; Lindsey, C. Bibcode: 1993BAAS...25.1181K Altcode: No abstract at ADS Title: A Magnetograph Comparison Workshop Authors: Jones, H.; Bogart, R.; Canfield, R.; Chapman, G.; Henney, C.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet, V.; Rabin, D.; Ulrich, R.; Walton, S. Bibcode: 1993BAAS...25.1216J Altcode: No abstract at ADS Title: Intercomparison of Seven Magnetographs Authors: Walton, S. R.; Bogart, R. S.; Chapman, G. A.; Henney, C.; Jones, H.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet, V.; Rabin, D. Bibcode: 1993BAAS...25.1205W Altcode: No abstract at ADS Title: Helioseismic Prospects in the Mid Infrared Authors: Kopp, G. Bibcode: 1993ASPC...42..473K Altcode: 1993gong.conf..473K No abstract at ADS Title: Thermal Images of Sunspots and the Quite Sun at 4.8, 12.4, and 18 microns Authors: Gezari, D.; Kopp, G.; Livingston, W. Bibcode: 1993AAS...181.8103G Altcode: 1993BAAS...25..733G No abstract at ADS Title: Submillimeter Solar Images from the JCMT Authors: Kopp, G.; Lindsey, C. Bibcode: 1992AAS...181.9406K Altcode: 1992BAAS...24.1270K We present nearly full-disk, diffraction-limited solar images made at 350 and 850 microns and at 1.3 mm from the 15 m James Clerk Maxwell Telescope on Mauna Kea. These wavelengths sample the thermal structure of the solar chromosphere at altitudes from 500 to about 1500 km, providing a height-dependent diagnostic of the atmosphere. Filament channels and neutral lines are apparent in the submillimeter images, although filaments themselves are not clearly visible. The submillimeter images show plage approximately 20% brighter than the surrounding quiet Sun, while sunspot intensities are comparable to the quiet Sun. ``Circumfacules,'' dark areas surrounding active regions, are observed in the submillimeter images and are similar to those seen in Ca 8542; comparison with Ca H and K may give estimates of the temperature and filling factor of the hot gas present in these probably bifurcated regions. Title: NIM --- A Near Infrared Magnetograph Authors: Rabin, D.; Jaksha, D.; Kopp, G.; Mahaffey, C. Bibcode: 1992AAS...181.8101R Altcode: 1992BAAS...24.1251R \newcommand{\micron}{microns} \newcommand{\kayser}{cm(-1) } \newcommand{\NIM}{NIM} We describe a new instrument for mapping magnetic field strength in the active solar photosphere. \NIM\ is a Stokes spectropolarimeter that exploits the high Zeeman sensitivity of the line Fe I 6388.64 \kayser\ (15648.5 Angstroms, e\:(7D_1) -- 3d(6) 4s 5p\:(7D^) o_1, Lande g = 3.00, chi_e = 5.36 eV) to measure vec {B}. For |B| ga 850 G, the magnitude of the field is derived, without adjustable parameters, from the complete splitting of the Zeeman components. The relative strengths of the Stokes components indicate the direction of the field. The absolute strength of the polarized signal depends on the areal filling factor, inclination, continuum contrast, and line strength of the magnetic flux tubes within the angular resolution element. \NIM\ comprises the following subsystems: precision image scanner liquid crystal polarization modulators and control electronics slit spectrograph transfer and minification optics 128 times 128 InSb infrared array camera computer for data acquisition and user interface \NIM\ builds up a two-dimensional array of polarized spectra by scanning the solar image across the spectrograph slit. The spatial and spectral sampling frequencies are 1.0 arcsec or 0.5 arcsec per pixel (depending on which telescope is used) and 0.025 \kayser\ per pixel. At each slit position, 8 polarization pairs for each Stokes parameter (e.g., +/- V) are acquired at 7 Hz, averaged, and recorded in FITS format. A 128 times 128 arcsec(2) map is acquired in about 20 minutes. \NIM\ is available to NSO visiting observers at the McMath-Pierce Telescope on Kitt Peak. Title: Thermal Maps of Sunspots and the Quiet Sun Authors: Livingston, W.; Kopp, G.; Gezari, D. Bibcode: 1992AAS...181.8103L Altcode: 1992BAAS...24.1252L We present images of sunspots, surrounding plage, quiet Sun, and the solar limb made at 4.8, 12.4, and 18 microns. These are basically thermal maps, the infrared intensity being nearly linearly proportional to temperature at these wavelengths. We believe these to be the most detailed thermal images to date of the solar photosphere. Thermal structure within sunspot penumbrae and the surrounding plage is evident in several images, although umbrae appear homogeneous, at least down to the approximately 2'' diffraction limit of the telescope at 12 microns. We find the temperature of penumbrae to be roughly 5% less than that of the quiet Sun, and umbrae to be about 25% less. Images of the quiet Sun show spatial thermal fluctuations of about 2% in patterns that change slowly with time. The measurements were made with the NSO's windowless, filled-aperture 1.6 m McMath-Pierce Solar Telescope, which fed the infrared image to a cryogenically-cooled 58x62 Si:Ge camera system built by D. Gezari. Title: A Relation Between Magnetic Field Strength and Temperature in Sunspots Authors: Kopp, Greg; Rabin, Douglas Bibcode: 1992SoPh..141..253K Altcode: We present Stokes I Zeeman splitting measurements of sunspots using the highly sensitive (g = 3) Fe I line at λ = 1.5649 μm. The splittings are compared with simultaneous intensity measurements in the adjacent continuum. The relation between magnetic field strength and temperature has a characteristic, nonlinear shape in all the spots studied. In the umbra, there is an approximately linear relation between B2 and Tb, consistent with magnetohydrostatic equilibrium in a nearly vertical field. A distinct flattening of the B2 vs Tbrelationship in the inner penumbra may be due to changes in the lateral pressure balance as the magnetic field becomes more horizontal; spatially unresolved intensity inhomogeneities may also influence the observed relation. Title: Infrared Determinations of Magnetic Profiles in Sunspots Authors: Kopp, G.; Kuhn, J.; Lin, H.; Rabin, D. Bibcode: 1992AAS...180.1202K Altcode: 1992BAAS...24R.747K We present measurements of a sunspot using unpolarized observations of the magnetically-sensitive (Lande g=3) Fe I line at lambda =1.5649 microns (6388.6 cm(-1) ). We compare the magnetic field profile from this fairly symmetric spot with model profiles. Splittings in this infrared line are nearly a factor of 3 greater than in a comparable visible line, since Zeeman splitting as a fraction of linewidth increases linearly with wavelength. The infrared is also less affected by stray light than the visible, because the intensity contrast is reduced, decreasing the effects of stray light, and because instrumental scatter is lower in the infrared. The combination of the magnetic and stray light advantages of the infrared and the recent availability of ``large'' infrared arrays has made possible more sensitive determinations of the magnetic field profile throughout sunspots. From observations of several sunspots, we find that the magnetic field strength, determined in the strong field regime, is not a smooth function of radius from spot center, and that single radial parameter models do not accurately describe the observed spots. Title: Chromospheric Dynamics Based on Infrared Solar Brightness Variations Authors: Kopp, G.; Lindsey, C.; Roellig, T. L.; Werner, M. W.; Becklin, E. E.; Orrall, F. Q.; Jefferies, J. T. Bibcode: 1992ApJ...388..203K Altcode: The NASA Kuiper Airborne Observatory was used to observe far-infrared continuum brightness fluctuations in the lower chromosphere due to solar 5 minute oscillations on the quiet sun. Brightness measurements made at 50, 100, 200, and 400 microns show a strong correlation with visible-line Doppler measurements from photospheric and chromospheric altitudes. The motion of the chromosphere is nearly in phase over a large range of heights, while the infrared brightness lags the Doppler velocity by phases varying from significantly less than 90 deg at low altitudes to nearly 90 deg at higher altitudes. It is proposed that this is the result of a nonadiabatic response of the chromospheric gas to compression and may indicate an important mechanism for wave dissipation. Thermal relaxation times ranging from about 40 s at 340 km above the tau(5000) = 1 photosphere to about 300 s at 600 km are proposed. Title: Submillimeter Solar Limb Profiles Determined from Observations of the Total Solar Eclipse of 1988 March 18 Authors: Roellig, T. L.; Becklin, E. E.; Jefferies, J. T.; Kopp, G. A.; Lindsey, C. A.; Orrall, F. Q.; Werner, M. W. Bibcode: 1991ApJ...381..288R Altcode: Observations were made of the extreme solar limb in six far-infrared wavelength bands ranging from 30 to 670 micron using the Kuiper Airborne Observatory during the total eclipse of the sun on 1988 March 18. By observations of the occultation of the solar limb by the moon, it was possible to obtain a spatial resolution of 0.5 arcsec normal to the limb. The solar limb was found to be extended with respect to the visible limb at all of these wavelengths, with the extension increasing with wavelength. Limb brightening was observed to increase slightly with increasing wavelength, and no sign of a sharp emission spike at the extreme limb was found at any of these wavelengths. The observations can be well fitted by a chromospheric model incorporating cool dense spicules in the lower chromosphere. Title: Zeeman Splitting and Continuum Measurements of Sunspots at 1.56 μm Authors: Kopp, G.; Rabin, D.; Lindsey, C. Bibcode: 1991BAAS...23.1055K Altcode: No abstract at ADS Title: Modelling of Chromospheric Dynamics Based on Infrared Solar Brightness Variations Authors: Kopp, G. Bibcode: 1990BAAS...22..896K Altcode: No abstract at ADS Title: Far-Infrared Intensity Variations Caused by 5 Minute Oscillations Authors: Lindsey, C.; Kopp, G.; Becklin, E. E.; Roellig, T.; Werner, M. W.; Jefferies, J. T.; Orrall, F. Q.; Braun, D.; Mickey, D. L. Bibcode: 1990ApJ...350..475L Altcode: Observations of solar IR intensity variations at 50, 100, and 200 microns were made simultaneously and cospatially with Doppler measurements in the sodium D1 line at 5896 A. Brightness temperature variations of several K in amplitude are highly correlated with five minute Doppler oscillations. The brightness variations are attributed to work done on the chromospheric medium by compression, driven by the five minute oscillations. The Doppler oscillations lead the brightness variations by about 47 deg in phase at 50 and 100 microns and by about 72 deg in phase at 200 microns. Title: Chromospheric Dynamics Based on Infrared Solar Brightness Variations Authors: Kopp, Greg Bibcode: 1990PhDT........10K Altcode: Infrared techniques were used to observe continuum emission from the solar chromosphere near temperature minimum in order to model the thermal response of the atmosphere to compressions due to 5-minute solar oscillations. Using one airborne and two ground-based observatories, simultaneous infrared intensity (temperature) and visible Doppler velocity measurements were acquired at several heights in the chromosphere, thus allowing comparisons between the motions of the atmospheric gas and the thermal fluctuations. While 5-minute oscillations in the lower chromosphere are frequently thought to be evanescent, so that the compression of the gas is in phase at all heights, the temperature changes due to these oscillations are found to vary in phase with altitude, implying the gas behaves non-adiabatically in this region. The phases between the velocities of the gas and the temperature fluctuations were determined at several heights near temperature minimum. The chromosphere was then modelled as a planar gravitationally-stratified gas with thermal relaxation toward an equilibrium, isothermal temperature permitted in the equation describing temperature change with compression. The rates of thermal relaxation at different altitudes were estimated from the observed phases between the infrared and visible data. The relaxation times were found to vary from 30 seconds at an altitude of 350 km above the photosphere to roughly 200 seconds at 600 km altitude. The effects of compression on the opacity of the gas were also studied, in order to predict the consequences of a non-isothermal atmosphere on the continuum observations. An estimate of the energy lost from solar oscillations due to thermal relaxation is calculated for the altitudes observed, and it appears that solar oscillations may be partially responsible for heating the lower chromosphere by thermal relaxation. Title: Profiles of the Extreme Solar Limb at Far Infrared and Submillimeter Wavelengths Authors: Roellig, T. L.; Werner, M. W.; Kopp, G.; Becklin, E. E.; Lindsey, C.; Orrall, F. Q.; Jefferies, J. T. Bibcode: 1989BAAS...21..765R Altcode: No abstract at ADS Title: Submillimeter Observations of the Extreme Solar Limb by Occultation in the Total Solar Eclipse of 18 March 1988 Authors: Roellig, T. R.; Werner, M. W.; Kopp, G.; Becklin, E. E.; Lindsey, C.; Orrall, F. Q.; Jefferies, J. T. Bibcode: 1988BAAS...20..689R Altcode: No abstract at ADS Title: Simultaneous Observations of Far-Infrared Solar Continuum Brightness Variations and Five-Minute Oscillations Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Kopp, G.; Werner, M. W.; Roellig, T. R. Bibcode: 1988BAAS...20..690L Altcode: No abstract at ADS Title: Modeling the Solar Chromosphere by Airborne Solar Eclipse Observations Authors: Orrall, F. Q.; Becklin, E. E.; Lindsey, C.; Roellig, T. R.; Werner, M. W.; Kopp, G.; Jefferies, J. T. Bibcode: 1987BAAS...19.1014O Altcode: No abstract at ADS Title: Observations of Far-Infrared Solar Continuum Variations Due to Compression Waves Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Werner, M. W.; Roellig, T. R.; Kopp, G.; Jefferies, J. T. Bibcode: 1987BAAS...19S1014L Altcode: No abstract at ADS Title: Observations of Far-Infrared Solar Continuum Variations Due to Compression Waves Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Werner, M. W.; Roellig, T. R.; Kopp, G. Bibcode: 1987BAAS...19R.933L Altcode: No abstract at ADS Title: Observations of far-infrared solar continuum variations due to compression waves. Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Werner, M. W.; Roellig, T. R.; Kopp, G. Bibcode: 1987BAAS...19..933L Altcode: No abstract at ADS Title: Observations of far-infrared solar continuum variations due to compression waves. Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Werner, M. W.; Roellig, T. R.; Kopp, G. Bibcode: 1987BAAS...19..741L Altcode: No abstract at ADS Title: Observations of Far-Infrared Solar Continuum Variations Due to Compression Waves Authors: Lindsey, C.; Becklin, E. E.; Orrall, F. Q.; Werner, M. W.; Roellig, T. R.; Kopp, G. Bibcode: 1987BAAS...19R.741L Altcode: No abstract at ADS