Author name code: goodman
ADS astronomy entries on 2022-09-14
author:"Goodman, Michael L." 
------------------------------------------------------------------------  

Title: Review of Particle Physics
Authors: Particle Data Group; Zyla, P. A.; Barnett, R. M.; Beringer,
   J.; Dahl, O.; Dwyer, D. A.; Groom, D. E.; Lin, C. -J.; Lugovsky,
   K. S.; Pianori, E.; Robinson, D. J.; Wohl, C. G.; Yao, W. -M.;
   Agashe, K.; Aielli, G.; Allanach, B. C.; Amsler, C.; Antonelli, M.;
   Aschenauer, E. C.; Asner, D. M.; Baer, H.; Banerjee, Sw; Baudis, L.;
   Bauer, C. W.; Beatty, J. J.; Belousov, V. I.; Bethke, S.; Bettini,
   A.; Biebel, O.; Black, K. M.; Blucher, E.; Buchmuller, O.; Burkert,
   V.; Bychkov, M. A.; Cahn, R. N.; Carena, M.; Ceccucci, A.; Cerri,
   A.; Chakraborty, D.; Chivukula, R. Sekhar; Cowan, G.; D'Ambrosio, G.;
   Damour, T.; de Florian, D.; de Gouvêa, A.; DeGrand, T.; de Jong, P.;
   Dissertori, G.; Dobrescu, B. A.; D'Onofrio, M.; Doser, M.; Drees, M.;
   Dreiner, H. K.; Eerola, P.; Egede, U.; Eidelman, S.; Ellis, J.; Erler,
   J.; Ezhela, V. V.; Fetscher, W.; Fields, B. D.; Foster, B.; Freitas,
   A.; Gallagher, H.; Garren, L.; Gerber, H. -J.; Gerbier, G.; Gershon,
   T.; Gershtein, Y.; Gherghetta, T.; Godizov, A. A.; Gonzalez-Garcia,
   M. C.; Goodman, M.; Grab, C.; Gritsan, A. V.; Grojean, C.; Grünewald,
   M.; Gurtu, A.; Gutsche, T.; Haber, H. E.; Hanhart, C.; Hashimoto, S.;
   Hayato, Y.; Hebecker, A.; Heinemeyer, S.; Heltsley, B.; Hernández-Rey,
   J. J.; Hikasa, K.; Hisano, J.; Höcker, A.; Holder, J.; Holtkamp, A.;
   Huston, J.; Hyodo, T.; Johnson, K. F.; Kado, M.; Karliner, M.; Katz,
   U. F.; Kenzie, M.; Khoze, V. A.; Klein, S. R.; Klempt, E.; Kowalewski,
   R. V.; Krauss, F.; Kreps, M.; Krusche, B.; Kwon, Y.; Lahav, O.; Laiho,
   J.; Lellouch, L. P.; Lesgourgues, J.; Liddle, A. R.; Ligeti, Z.;
   Lippmann, C.; Liss, T. M.; Littenberg, L.; Lourengo, C.; Lugovsky,
   S. B.; Lusiani, A.; Makida, Y.; Maltoni, F.; Mannel, T.; Manohar,
   A. V.; Marciano, W. J.; Masoni, A.; Matthews, J.; Meißner, U. -G.;
   Mikhasenko, M.; Miller, D. J.; Milstead, D.; Mitchell, R. E.; Mönig,
   K.; Molaro, P.; Moortgat, F.; Moskovic, M.; Nakamura, K.; Narain, M.;
   Nason, P.; Navas, S.; Neubert, M.; Nevski, P.; Nir, Y.; Olive, K. A.;
   Patrignani, C.; Peacock, J. A.; Petcov, S. T.; Petrov, V. A.; Pich,
   A.; Piepke, A.; Pomarol, A.; Profumo, S.; Quadt, A.; Rabbertz, K.;
   Rademacker, J.; Raffelt, G.; Ramani, H.; Ramsey-Musolf, M.; Ratcliff,
   B. N.; Richardson, P.; Ringwald, A.; Roesler, S.; Rolli, S.; Romaniouk,
   A.; Rosenberg, L. J.; Rosner, J. L.; Rybka, G.; Ryskin, M.; Ryutin,
   R. A.; Sakai, Y.; Salam, G. P.; Sarkar, S.; Sauli, F.; Schneider, O.;
   Scholberg, K.; Schwartz, A. J.; Schwiening, J.; Scott, D.; Sharma,
   V.; Sharpe, S. R.; Shutt, T.; Silari, M.; Sjöstrand, T.; Skands,
   P.; Skwarnicki, T.; Smoot, G. F.; Soffer, A.; Sozzi, M. S.; Spanier,
   S.; Spiering, C.; Stahl, A.; Stone, S. L.; Sumino, Y.; Sumiyoshi, T.;
   Syphers, M. J.; Takahashi, F.; Tanabashi, M.; Tanaka, J.; Taševský,
   M.; Terashi, K.; Terning, J.; Thoma, U.; Thorne, R. S.; Tiator, L.;
   Titov, M.; Tkachenko, N. P.; Tovey, D. R.; Trabelsi, K.; Urquijo, P.;
   Valencia, G.; Van de Water, R.; Varelas, N.; Venanzoni, G.; Verde,
   L.; Vincter, M. G.; Vogel, P.; Vogelsang, W.; Vogt, A.; Vorobyev,
   V.; Wakely, S. P.; Walkowiak, W.; Walter, C. W.; Wands, D.; Wascko,
   M. O.; Weinberg, D. H.; Weinberg, E. J.; White, M.; Wiencke, L. R.;
   Willocq, S.; Woody, C. L.; Workman, R. L.; Yokoyama, M.; Yoshida,
   R.; Zanderighi, G.; Zeller, G. P.; Zenin, O. V.; Zhu, R. -Y.; Zhu,
   S. -L.; Zimmermann, F.; Anderson, J.; Basaglia, T.; Lugovsky, V. S.;
   Schaffner, P.; Zheng, W.
Bibcode: 2020PTEP.2020h3C01P
Altcode:
  The Review summarizes much of particle physics and cosmology. Using data
  from previous editions, plus 3,324 new measurements from 878 papers,
  we list, evaluate, and average measured properties of gauge bosons
  and the recently discovered Higgs boson, leptons, quarks, mesons,
  and baryons. We summarize searches for hypothetical particles such
  as supersymmetric particles, heavy bosons, axions, dark photons,
  etc. Particle properties and search limits are listed in Summary
  Tables. We give numerous tables, figures, formulae, and reviews of
  topics such as Higgs Boson Physics, Supersymmetry, Grand Unified
  Theories, Neutrino Mixing, Dark Energy, Dark Matter, Cosmology,
  Particle Detectors, Colliders, Probability and Statistics. Among
  the 120 reviews are many that are new or heavily revised, including
  a new review on High Energy Soft QCD and Diffraction and one on the
  Determination of CKM Angles from B Hadrons.

Title: A new approach to solar flare prediction
Authors: Goodman, Michael L.; Kwan, Chiman; Ayhan, Bulent; Shang,
   Eric L.
Bibcode: 2020FrPhy..1534601G
Altcode: 2020arXiv200301823G
  All three components of the current density are required to compute
  the heating rate due to free magnetic energy dissipation. Here we
  present a first test of a new model developed to determine if the
  times of increases in the resistive heating rate in active region
  (AR) photospheres are correlated with the subsequent occurrence
  of M and X flares in the corona. A data driven, 3D, non-force-free
  magnetohydrodynamic model restricted to the near-photospheric region
  is used to compute time series of the complete current density and the
  resistive heating rate per unit volume [Q(t)] in each pixel in neutral
  line regions (NLRs) of 14 ARs. The model is driven by time series
  of the magnetic field B measured by the Helioseismic & Magnetic
  Imager on the Solar Dynamics Observatory (SDO) satellite. Spurious
  Doppler periods due to SDO orbital motion are filtered out of the
  time series for B in every AR pixel. For each AR, the cumulative
  distribution function (CDF) of the values of the NLR area integral
  Q<SUB>i</SUB>(t) of Q(t) is found to be a scale invariant power law
  distribution essentially identical to the observed CDF for the total
  energy released in coronal flares. This suggests that coronal flares
  and the photospheric Q<SUB>i</SUB> are correlated, and powered by the
  same process. The model predicts spikes in Q<SUB>i</SUB> with values
  orders of magnitude above background values. These spikes are driven
  by spikes in the non-force free component of the current density. The
  times of these spikes are plausibly correlated with times of subsequent
  M or X flares a few hours to a few days later. The spikes occur on
  granulation scales, and may be signatures of heating in horizontal
  current sheets. It is also found that the times of relatively large
  values of the rate of change of the NLR unsigned magnetic flux are
  also plausibly correlated with the times of subsequent M and X flares,
  and spikes in Q<SUB>i</SUB>.

Title: Review of Particle Physics<SUP>*</SUP>
Authors: Tanabashi, M.; Hagiwara, K.; Hikasa, K.; Nakamura, K.; Sumino,
   Y.; Takahashi, F.; Tanaka, J.; Agashe, K.; Aielli, G.; Amsler, C.;
   Antonelli, M.; Asner, D. M.; Baer, H.; Banerjee, Sw.; Barnett, R. M.;
   Basaglia, T.; Bauer, C. W.; Beatty, J. J.; Belousov, V. I.; Beringer,
   J.; Bethke, S.; Bettini, A.; Bichsel, H.; Biebel, O.; Black, K. M.;
   Blucher, E.; Buchmuller, O.; Burkert, V.; Bychkov, M. A.; Cahn, R. N.;
   Carena, M.; Ceccucci, A.; Cerri, A.; Chakraborty, D.; Chen, M. -C.;
   Chivukula, R. S.; Cowan, G.; Dahl, O.; D'Ambrosio, G.; Damour, T.;
   de Florian, D.; de Gouvêa, A.; DeGrand, T.; de Jong, P.; Dissertori,
   G.; Dobrescu, B. A.; D'Onofrio, M.; Doser, M.; Drees, M.; Dreiner,
   H. K.; Dwyer, D. A.; Eerola, P.; Eidelman, S.; Ellis, J.; Erler, J.;
   Ezhela, V. V.; Fetscher, W.; Fields, B. D.; Firestone, R.; Foster, B.;
   Freitas, A.; Gallagher, H.; Garren, L.; Gerber, H. -J.; Gerbier, G.;
   Gershon, T.; Gershtein, Y.; Gherghetta, T.; Godizov, A. A.; Goodman,
   M.; Grab, C.; Gritsan, A. V.; Grojean, C.; Groom, D. E.; Grünewald,
   M.; Gurtu, A.; Gutsche, T.; Haber, H. E.; Hanhart, C.; Hashimoto, S.;
   Hayato, Y.; Hayes, K. G.; Hebecker, A.; Heinemeyer, S.; Heltsley, B.;
   Hernández-Rey, J. J.; Hisano, J.; Höcker, A.; Holder, J.; Holtkamp,
   A.; Hyodo, T.; Irwin, K. D.; Johnson, K. F.; Kado, M.; Karliner, M.;
   Katz, U. F.; Klein, S. R.; Klempt, E.; Kowalewski, R. V.; Krauss, F.;
   Kreps, M.; Krusche, B.; Kuyanov, Yu. V.; Kwon, Y.; Lahav, O.; Laiho,
   J.; Lesgourgues, J.; Liddle, A.; Ligeti, Z.; Lin, C. -J.; Lippmann, C.;
   Liss, T. M.; Littenberg, L.; Lugovsky, K. S.; Lugovsky, S. B.; Lusiani,
   A.; Makida, Y.; Maltoni, F.; Mannel, T.; Manohar, A. V.; Marciano,
   W. J.; Martin, A. D.; Masoni, A.; Matthews, J.; Meißner, U. -G.;
   Milstead, D.; Mitchell, R. E.; Mönig, K.; Molaro, P.; Moortgat, F.;
   Moskovic, M.; Murayama, H.; Narain, M.; Nason, P.; Navas, S.; Neubert,
   M.; Nevski, P.; Nir, Y.; Olive, K. A.; Pagan Griso, S.; Parsons, J.;
   Patrignani, C.; Peacock, J. A.; Pennington, M.; Petcov, S. T.; Petrov,
   V. A.; Pianori, E.; Piepke, A.; Pomarol, A.; Quadt, A.; Rademacker, J.;
   Raffelt, G.; Ratcliff, B. N.; Richardson, P.; Ringwald, A.; Roesler,
   S.; Rolli, S.; Romaniouk, A.; Rosenberg, L. J.; Rosner, J. L.; Rybka,
   G.; Ryutin, R. A.; Sachrajda, C. T.; Sakai, Y.; Salam, G. P.; Sarkar,
   S.; Sauli, F.; Schneider, O.; Scholberg, K.; Schwartz, A. J.; Scott,
   D.; Sharma, V.; Sharpe, S. R.; Shutt, T.; Silari, M.; Sjöstrand,
   T.; Skands, P.; Skwarnicki, T.; Smith, J. G.; Smoot, G. F.; Spanier,
   S.; Spieler, H.; Spiering, C.; Stahl, A.; Stone, S. L.; Sumiyoshi,
   T.; Syphers, M. J.; Terashi, K.; Terning, J.; Thoma, U.; Thorne,
   R. S.; Tiator, L.; Titov, M.; Tkachenko, N. P.; Törnqvist, N. A.;
   Tovey, D. R.; Valencia, G.; Van de Water, R.; Varelas, N.; Venanzoni,
   G.; Verde, L.; Vincter, M. G.; Vogel, P.; Vogt, A.; Wakely, S. P.;
   Walkowiak, W.; Walter, C. W.; Wands, D.; Ward, D. R.; Wascko, M. O.;
   Weiglein, G.; Weinberg, D. H.; Weinberg, E. J.; White, M.; Wiencke,
   L. R.; Willocq, S.; Wohl, C. G.; Womersley, J.; Woody, C. L.; Workman,
   R. L.; Yao, W. -M.; Zeller, G. P.; Zenin, O. V.; Zhu, R. -Y.; Zhu,
   S. -L.; Zimmermann, F.; Zyla, P. A.; Anderson, J.; Fuller, L.;
   Lugovsky, V. S.; Schaffner, P.; Particle Data Group
Bibcode: 2018PhRvD..98c0001T
Altcode:
  The Review summarizes much of particle physics and cosmology. Using data
  from previous editions, plus 2,873 new measurements from 758 papers,
  we list, evaluate, and average measured properties of gauge bosons
  and the recently discovered Higgs boson, leptons, quarks, mesons,
  and baryons. We summarize searches for hypothetical particles such
  as supersymmetric particles, heavy bosons, axions, dark photons,
  etc. Particle properties and search limits are listed in Summary
  Tables. We give numerous tables, figures, formulae, and reviews
  of topics such as Higgs Boson Physics, Supersymmetry, Grand Unified
  Theories, Neutrino Mixing, Dark Energy, Dark Matter, Cosmology, Particle
  Detectors, Colliders, Probability and Statistics. Among the 118 reviews
  are many that are new or heavily revised, including a new review on
  Neutrinos in Cosmology. <P />Starting with this edition, the Review
  is divided into two volumes. Volume 1 includes the Summary Tables and
  all review articles. Volume 2 consists of the Particle Listings. Review
  articles that were previously part of the Listings are now included in
  volume 1. <P />The complete Review (both volumes) is published online
  on the website of the Particle Data Group (http://pdg.lbl.gov) and in
  a journal. Volume 1 is available in print as the PDG Book. A Particle
  Physics Booklet with the Summary Tables and essential tables, figures,
  and equations from selected review articles is also available. <P />The
  2018 edition of the Review of Particle Physics should be cited as:
  M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98, 030001
  (2018).

Title: Cosmic-muon characterization and annual modulation measurement
    with Double Chooz detectors
Authors: Abrahão, T.; Almazan, H.; dos Anjos, J. C.; Appel, S.;
   Baussan, E.; Bekman, I.; Bezerra, T. J. C.; Bezrukov, L.; Blucher,
   E.; Brugière, T.; Buck, C.; Busenitz, J.; Cabrera, A.; Camilleri,
   L.; Carr, R.; Cerrada, M.; Chauveau, E.; Chimenti, P.; Corpace,
   O.; Crespo-Anadón, J. I.; Dawson, J. V.; Dhooghe, J.; Djurcic, Z.;
   Dracos, M.; Etenko, A.; Fallot, M.; Franco, D.; Franke, M.; Furuta,
   H.; Gil-Botella, I.; Giot, L.; Givaudan, A.; Gögger-Neff, M.; Gómez,
   H.; Gonzalez, L. F. G.; Goodman, M.; Hara, T.; Haser, J.; Hellwig,
   D.; Hourlier, A.; Ishitsuka, M.; Jochum, J.; Jollet, C.; Kale, K.;
   Kampmann, P.; Kaneda, M.; Kaplan, D. M.; Kawasaki, T.; Kemp, E.; de
   Kerret, H.; Kryn, D.; Kuze, M.; Lachenmaier, T.; Lane, C.; Laserre, T.;
   Lastoria, C.; Lhuillier, D.; Lima, H.; Lindner, M.; López-Castaño,
   J. M.; LoSecco, J. M.; Lubsandorzhiev, B.; Maeda, J.; Mariani, C.;
   Maricic, J.; Matsubara, T.; Mention, G.; Meregaglia, A.; Miletic, T.;
   Minotti, A.; Nagasaka, Y.; Navas-Nicolás, D.; Novella, P.; Oberauer,
   L.; Obolensky, M.; Onillon, A.; Oralbaev, A.; Palomares, C.; Pepe,
   I.; Pronost, G.; Reinhold, B.; Rybolt, B.; Sakamoto, Y.; Santorelli,
   R.; Schönert, S.; Schoppmann, S.; Sharankova, R.; Sibille, V.; Sinev,
   V.; Skorokhvatov, M.; Soiron, M.; Soldin, P.; Stahl, A.; Stancu, I.;
   Stokes, L. F. F.; Strait, M.; Suekane, F.; Sukhotin, S.; Sumiyoshi,
   T.; Sun, Y.; Svoboda, B.; Tonazzo, A.; Veyssiere, C.; Vivier, M.;
   Wagner, S.; Wiebusch, C.; Wurm, M.; Yang, G.; Yermia, F.; Zimmer, V.
Bibcode: 2017JCAP...02..017A
Altcode: 2016arXiv161107845A
  A study on cosmic muons has been performed for the two identical
  near and far neutrino detectors of the Double Chooz experiment,
  placed at ~120 and ~300 m.w.e. underground respectively,
  including the corresponding simulations using the MUSIC simulation
  package. This characterization has allowed us to measure the muon
  flux reaching both detectors to be (3.64 ± 0.04) × 10<SUP>-4</SUP>
  cm<SUP>-2</SUP>s<SUP>-1</SUP> for the near detector and (7.00 ± 0.05)
  × 10<SUP>-5</SUP> cm<SUP>-2</SUP>s<SUP>-1</SUP> for the far one. The
  seasonal modulation of the signal has also been studied observing a
  positive correlation with the atmospheric temperature, leading to an
  effective temperature coefficient of α<SUB>T</SUB> = 0.212 ± 0.024
  and 0.355 ± 0.019 for the near and far detectors respectively. These
  measurements, in good agreement with expectations based on theoretical
  models, represent one of the first measurements of this coefficient
  in shallow depth installations.

Title: Seasonal Variation of Multiple-Muon Events in MINOS and NOvA
Authors: Habig, A.; Goodman, M.; Schreiner, P.; Tognini, S.; Gomes,
   R.; Minos Collaboration; Nova Collaboration
Bibcode: 2017ICRC...35..200H
Altcode: 2017PoS...301..200H
  No abstract at ADS

Title: Neutrino Oscillations in the NOvA experiment
Authors: Habig, A.; Goodman, M.; NOvA Collaboration
Bibcode: 2017ICRC...35.1023H
Altcode: 2017PoS...301.1023H
  No abstract at ADS

Title: Photospheric Current Spikes And Their Possible Association
    With Flares - Results from an HMI Data Driven Model
Authors: Goodman, M. L.; Kwan, C.; Ayhan, B.; Eric, S. L.
Bibcode: 2016AGUFMSH31B2562G
Altcode:
  A data driven, near photospheric magnetohydrodynamic model predicts
  spikes in the horizontal current density, and associated resistive
  heating rate. The spikes appear as increases by orders of magnitude
  above background values in neutral line regions (NLRs) of active regions
  (ARs). The largest spikes typically occur a few hours to a few days
  prior to M or X flares. The spikes correspond to large vertical
  derivatives of the horizontal magnetic field. The model takes as
  input the photospheric magnetic field observed by the Helioseismic
  &amp; Magnetic Imager (HMI) on the Solar Dynamics Observatory
  (SDO) satellite. This 2.5 D field is used to determine an analytic
  expression for a 3 D magnetic field, from which the current density,
  vector potential, and electric field are computed in every AR pixel
  for 14 ARs. The field is not assumed to be force-free. The spurious 6,
  12, and 24 hour Doppler periods due to SDO orbital motion are filtered
  out of the time series of the HMI magnetic field for each pixel. The
  subset of spikes analyzed at the pixel level are found to occur on
  HMI and granulation scales of 1 arcsec and 12 minutes. Spikes are
  found in ARs with and without M or X flares, and outside as well as
  inside NLRs, but the largest spikes are localized in the NLRs of ARs
  with M or X flares. The energy to drive the heating associated with
  the largest current spikes comes from bulk flow kinetic energy, not
  the electromagnetic field, and the current density is highly non-force
  free. The results suggest that, in combination with the model, HMI is
  revealing strong, convection driven, non-force free heating events on
  granulation scales, and it is plausible these events are correlated
  with subsequent M or X flares. More and longer time series need to be
  analyzed to determine if such a correlation exists.

Title: Basic Properties of Plasma-Neutral Coupling in the Solar
    Atmosphere
Authors: Goodman, Michael
Bibcode: 2015TESS....140001G
Altcode:
  Plasma-neutral coupling (PNC) in the solar atmosphere concerns the
  effects of collisions between charged and neutral species’. It
  is most important in the chromosphere, which is the weakly ionized,
  strongly magnetized region between the weakly ionized, weakly magnetized
  photosphere and the strongly ionized, strongly magnetized corona. The
  charged species’ are mainly electrons, protons, and singly charged
  heavy ions. The neutral species’ are mainly hydrogen and helium. The
  resistivity due to PNC can be several orders of magnitude larger than
  the Spitzer resistivity. This enhanced resistivity is confined to the
  chromosphere, and provides a highly efficient dissipation mechanism
  unique to the chromosphere. PNC may play an important role in many
  processes such as heating and acceleration of plasma; wave generation,
  propagation, and dissipation; magnetic reconnection; maintaining the
  near force-free state of the corona; and limiting mass flux into the
  corona. It might play a major role in chromospheric heating, and be
  responsible for the existence of the chromosphere as a relatively thin
  layer of plasma that emits a net radiative flux 10-100 times greater
  than that of the overlying corona. The required heating rate might
  be generated by Pedersen current dissipation triggered by the rapid
  increase of magnetization with height in the lower chromosphere,
  where most of the net radiative flux is emitted. Relatively cool
  regions of the chromosphere might be regions of minimal Pedersen
  current dissipation due to smaller magnetic field strength or
  perpendicular current density. This talk will discuss PNC from an MHD
  point of view, and focus on the basic parameters that determine its
  effectiveness. These parameters are ionization fraction, magnetization,
  and the electric field that drives current perpendicular to the
  magnetic field. By influencing this current and the electric field
  that drives it, PNC directly influences the rate at which energy is
  exchanged between the electromagnetic field and particles. In this
  way, PNC can have a strong influence on the energetics of a process
  that involves the conversion of magnetic energy into particle energy,
  which subsequently appears as radiation, waves, bulk flow, and heating.

Title: Acceleration of Type 2 Spicules in the Solar
    Chromosphere. II. Viscous Braking and Upper Bounds on Coronal
    Energy Input
Authors: Goodman, Michael L.
Bibcode: 2014ApJ...785...87G
Altcode: 2014arXiv1403.2694G
  A magnetohydrodynamic model is used to determine conditions under which
  the Lorentz force accelerates plasma to type 2 spicule speeds in the
  chromosphere. The model generalizes a previous model to include a more
  realistic pre-spicule state, and the vertical viscous force. Two cases
  of acceleration under upper chromospheric conditions are considered. The
  magnetic field strength for these cases is &lt;=12.5 and 25 G. Plasma is
  accelerated to terminal vertical speeds of 66 and 78 km s<SUP>-1</SUP>
  in 100 s, compared with 124 and 397 km s<SUP>-1</SUP> for the
  case of zero viscosity. The flows are localized within horizontal
  diameters ~80 and 50 km. The total thermal energy generated by viscous
  dissipation is ~10 times larger than that due to Joule dissipation,
  but the magnitude of the total cooling due to rarefaction is &gt;~
  this energy. Compressive heating dominates during the early phase of
  acceleration. The maximum energy injected into the corona by type 2
  spicules, defined as the energy flux in the upper chromosphere, may
  largely balance total coronal energy losses in quiet regions, possibly
  also in coronal holes, but not in active regions. It is proposed that
  magnetic flux emergence in intergranular regions drives type 2 spicules.

Title: Acceleration of Type II Spicules in the Solar Chromosphere
Authors: Goodman, M. L.
Bibcode: 2012AGUFMSH33D2258G
Altcode:
  A 2.5 D, time dependent magnetohydrodynamic model is used to test the
  proposition that observed type II spicule velocities can be generated
  by a Lorentz force under chromospheric conditions, and that maximum
  vertical flow speeds can be comparable to slow solar wind speeds
  ∼ 200-400 km/sec. It is found that current densities localized on
  observed space and time scales of type II spicules, and that generate
  maximum magnetic field strengths ≤ 50 G can generate a Lorentz force
  that accelerates plasma to terminal velocities similar to those of
  type II spicules. The maximum vertical flow speeds are ∼ 150-460
  km-sec<SUP>-1</SUP>, and horizontally localized within ∼ 2.5-10 km
  from the vertical axis of the spicule, suggesting that significant
  solar wind acceleration occurs in type II spicules on sub-resolution,
  horizontal spatial scales. Vertical flow speeds with Mach numbers
  &gt; ∼ 5 extend over horizontal regions with diameters ∼ 25-50
  km. Horizontal speeds are ∼ 20 times smaller than maximum vertical
  speeds. The increase in the mechanical and thermal energy of the plasma
  during the acceleration process is 2-3 × 10<SUP>22</SUP> ergs, which
  is ∼ 5 times smaller than nanoflare energies. The radial component of
  the Lorentz force compresses the plasma during the acceleration process
  by factors as large as ∼ 100. The Joule heating flux generated during
  this process is essentially due to proton Pedersen current dissipation,
  and can be ∼ 0.1 - 3.7 times the heating flux of ∼ 10<SUP>6</SUP>
  ergs-cm<SUP>-2</SUP>-s<SUP>-1</SUP> associated with middle-upper
  chromospheric emission. The maximum heating rate and vertical flow speed
  are respectively reached ∼ 23 s and 100 s after acceleration begins,
  indicating that most heating occurs well before terminal velocity
  is reached. About 84-94% of the magnetic energy that accelerates and
  heats the spicules is converted into bulk flow kinetic energy.

Title: Acceleration of Type II Spicules in the Solar Chromosphere
Authors: Goodman, Michael L.
Bibcode: 2012ApJ...757..188G
Altcode:
  A 2.5D, time-dependent magnetohydrodynamic model is used to test the
  proposition that observed type II spicule velocities can be generated
  by a Lorentz force under chromospheric conditions. It is found that
  current densities localized on observed space and time scales of type
  II spicules and that generate maximum magnetic field strengths &lt;=50
  G can generate a Lorentz force that accelerates plasma to terminal
  velocities similar to those of type II spicules. Maximum vertical flow
  speeds are ~150-460 km s<SUP>-1</SUP>, horizontally localized within
  ~2.5-10 km from the vertical axis of the spicule, and comparable
  to slow solar wind speeds, suggesting that significant solar wind
  acceleration occurs in type II spicules. Horizontal speeds are ~20
  times smaller than vertical speeds. Terminal velocity is reached ~100 s
  after acceleration begins. The increase in the mechanical and thermal
  energy of the plasma during acceleration is (2-3) × 10<SUP>22</SUP>
  ergs. The radial component of the Lorentz force compresses the plasma
  during the acceleration process by factors as large as ~100. The
  Joule heating flux generated during this process is essentially due
  to proton Pedersen current dissipation and can be ~0.1-3.7 times the
  heating flux of ~10<SUP>6</SUP> ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>
  associated with middle-upper chromospheric emission. About 84%-94%
  of the magnetic energy that accelerates and heats the spicules is
  converted into bulk flow kinetic energy.

Title: Radiating Current Sheets in the Solar Chromosphere
Authors: Goodman, Michael L.; Judge, Philip G.
Bibcode: 2012ApJ...751...75G
Altcode: 2014arXiv1406.1211G
  An MHD model of a hydrogen plasma with flow, an energy equation,
  NLTE ionization and radiative cooling, and an Ohm's law with
  anisotropic electrical conduction and thermoelectric effects
  is used to self-consistently generate atmospheric layers over a
  50 km height range. A subset of these solutions contains current
  sheets and has properties similar to those of the lower and middle
  chromosphere. The magnetic field profiles are found to be close to
  Harris sheet profiles, with maximum field strengths ~25-150 G. The
  radiative flux F<SUB>R</SUB> emitted by individual sheets is ~4.9 ×
  10<SUP>5</SUP>-4.5 × 10<SUP>6</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>,
  to be compared with the observed chromospheric emission rate of
  ~10<SUP>7</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>. Essentially all
  emission is from regions with thicknesses ~0.5-13 km containing the
  neutral sheet. About half of F<SUB>R</SUB> comes from sub-regions with
  thicknesses 10 times smaller. A resolution &lt;~ 5-130 m is needed to
  resolve the properties of the sheets. The sheets have total H densities
  ~10<SUP>13</SUP>-10<SUP>15</SUP> cm<SUP>-3</SUP>. The ionization
  fraction in the sheets is ~2-20 times larger, and the temperature is
  ~2000-3000 K higher than in the surrounding plasma. The Joule heating
  flux F<SUB>J</SUB> exceeds F<SUB>R</SUB> by ~4%-34%, the difference
  being balanced in the energy equation mainly by a negative compressive
  heating flux. Proton Pedersen current dissipation generates ~62%-77%
  of the positive contribution to F<SUB>J</SUB> . The remainder of this
  contribution is due to electron current dissipation near the neutral
  sheet where the plasma is weakly magnetized.

Title: Radiating Current Sheets in the Solar Chromosphere
Authors: Goodman, Michael L.; Judge, P. G.
Bibcode: 2012AAS...22052116G
Altcode:
  An MHD model of a Hydrogen plasma with flow, an energy equation,
  NLTE ionization and radiative cooling, and an Ohm's law with
  anisotropic electrical conduction and thermoelectric effects is used
  to self-consistently generate atmospheric layers over a 50 km height
  range. A subset of these solutions contain current sheets, and have
  properties similar to those of the lower and middle chromosphere. The
  magnetic field profiles are found to be close to Harris sheet profiles,
  with maximum field strengths 25-150 G. The radiative flux F_R emitted
  by individual sheets is 4.9 x 10^5 - 4.5 x 10^6 ergs-cm^{-2}-s^{-1},
  to be compared with the observed chromospheric emission rate of 10^7
  ergs-cm^{-2}-s^{-1}. Essentially all emission is from regions with
  thicknesses 0.5 - 13 km containing the neutral sheet. About half of F_R
  comes from sub-regions with thicknesses 10 times smaller. A resolution
  &lt; 5-130 m is needed to resolve the properties of the sheets. The
  sheets have total H densities 10^{13}-10^{15} cm^{-3}. The ionization
  fraction in the sheets is 2-20 times larger, and the temperature is
  2000-3000 K higher than in the surrounding plasma. The Joule heating
  flux F_J exceeds F_R by 4-34 %, the difference being balanced
  in the energy equation mainly by a negative compressive heating
  flux. Proton Pedersen current dissipation generates 62-77 % of the
  positive contribution to F_J. The remainder of this contribution
  is due to electron current dissipation near the neutral sheet where
  the plasma is weakly magnetized. These solutions represent the first,
  first principles theoretical proof of the existence of radiating current
  sheets under chromospheric conditions. The existence of these solutions
  suggests the existence of sub-resolution, horizontal current sheets
  in the chromosphere that are sites of strong Joule heating driven
  radiative emission.

Title: Conditions for Photospherically Driven Alfvénic Oscillations
    to Heat the Solar Chromosphere by Pedersen Current Dissipation
Authors: Goodman, Michael L.
Bibcode: 2011ApJ...735...45G
Altcode: 2014arXiv1410.8519G
  A magnetohydrodynamic model that includes a complete electrical
  conductivity tensor is used to estimate conditions for photospherically
  driven, linear, non-plane Alfvénic oscillations extending from the
  photosphere to the lower corona to drive a chromospheric heating rate
  due to Pedersen current dissipation that is comparable to the observed
  net chromospheric radiative loss of ~10<SUP>7</SUP> erg cm<SUP>-2</SUP>
  s<SUP>-1</SUP>. The heating rates due to electron current dissipation
  in the photosphere and corona are also computed. The wave amplitudes
  are computed self-consistently as functions of an inhomogeneous
  background (BG) atmosphere. The effects of the conductivity
  tensor are resolved numerically using a resolution of 3.33 m. The
  oscillations drive a chromospheric heating flux F <SUB>Ch</SUB>
  ~ 10<SUP>7</SUP>-10<SUP>8</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>
  at frequencies ν ~ 10<SUP>2</SUP>-10<SUP>3</SUP> mHz for BG magnetic
  field strengths B &gt;~ 700 G and magnetic field perturbation amplitudes
  ~0.01-0.1 B. The total resistive heating flux increases with ν. Most
  heating occurs in the photosphere. Thermalization of Poynting flux
  in the photosphere due to electron current dissipation regulates the
  Poynting flux into the chromosphere, limiting F <SUB>Ch</SUB>. F
  <SUB>Ch</SUB> initially increases with ν, reaches a maximum, and
  then decreases with increasing ν due to increasing electron current
  dissipation in the photosphere. The resolution needed to resolve the
  oscillations increases from ~10 m in the photosphere to ~10 km in the
  upper chromosphere and is vpropν<SUP>-1/2</SUP>. Estimates suggest
  that these oscillations are normal modes of photospheric flux tubes
  with diameters ~10-20 km, excited by magnetic reconnection in current
  sheets with thicknesses ~0.1 km.

Title: Conditions for Photospherically Driven Aflvenic Oscillations
    to Heat the Chromosphere by Pedersen Current Dissipation
Authors: Goodman, Michael L.
Bibcode: 2011SPD....42.1704G
Altcode: 2011BAAS..43S.1704G
  An MHD model that includes a complete electrical conductivity
  tensor is used to estimate conditions for photospherically
  driven, linear, non-plane Alfvenic oscillations extending from the
  photosphere to the lower corona to drive a chromospheric heating
  rate due to Pedersen current dissipation that is comparable
  to the observed net chromospheric radiative loss of 10<SUP>7
  </SUP>ergs-cm<SUP>-2</SUP>-sec<SUP>-1</SUP>. The heating rates due
  to electron current dissipation in the photosphere and corona are
  also computed. The wave amplitudes are computed self-consistently as
  functions of an inhomogeneous background atmosphere. The effects of the
  conductivity tensor are resolved numerically using a resolution of 3.33
  m. The oscillations drive a chromospheric heating flux F<SUB>Ch</SUB>
  10<SUP>7</SUP>-10<SUP>8</SUP> ergs-cm<SUP>-2</SUP>-sec<SUP>-1</SUP>
  at frequencies nu 10<SUP>2</SUP> - 10<SUP>3</SUP> mHz for background
  magnetic field strengths B &gt; 700 G, and magnetic field perturbation
  amplitudes 0.01-0.1 B. The total resistive heating flux increases
  with nu. Most heating occurs in the photosphere. Thermalization
  of Poynting flux in the photosphere due to electron current
  dissipation regulates the Poynting flux into the chromosphere,
  limiting F<SUB>Ch</SUB>. F<SUB>Ch</SUB> initially increases with
  nu, reaches a maximum, and then decreases with increasing nu due
  to increasing electron current dissipation in the photosphere. The
  resolution needed to resolve the oscillations increases from 10 m in
  the photosphere to 10 km in the upper chromosphere, and is proportional
  to nu<SUP>-1/2</SUP>. Estimates suggest these oscillations are normal
  modes of photospheric flux tubes with diameters 10-20 km, excited by
  magnetic reconnection in current sheets with thicknesses 0.1 km. <P
  />This work was supported by the NSF Solar Terrestrial Physics
  Program. It is described in detail in a paper in submission to ApJ.

Title: Analytic Solutions for Current Sheet Structure Determined by
    Self-consistent, Anisotropic Transport Processes in a Gravitational
    Field
Authors: Goodman, Michael L.
Bibcode: 2011ApJ...731...19G
Altcode:
  A Harris sheet magnetic field with maximum magnitude B <SUB>0</SUB> and
  length scale L is combined with the anisotropic electrical conductivity,
  viscosity, and thermoelectric tensors for an electron-proton plasma to
  define a magnetohydrodynamic model that determines the steady state of
  the plasma. The transport tensors are functions of temperature, density,
  and magnetic field strength, and are computed self-consistently as
  functions of position x normal to the current sheet. The flow velocity,
  magnetic field, and gravitational force lie along the z-axis. The plasma
  is supported against gravity by the viscous force. Analytic solutions
  are obtained for temperature, density, and velocity. They are valid
  over a broad range of temperature, density, and magnetic field strength,
  and so may be generally useful in astrophysical applications. Numerical
  examples of solutions in the parameter range of the solar atmosphere
  are presented. The objective is to compare Joule and viscous heating
  rates, determine the velocity shear that generates viscous forces that
  support the plasma and are self-consistent with a mean outward mass flux
  comparable to the solar wind mass flux, and compare the thermoelectric
  and conduction current contributions to the Joule heating rate. The
  ratio of the viscous to Joule heating rates per unit mass can exceed
  unity by orders of magnitude, and increases rapidly with L. The viscous
  heating rate can be concentrated outside the region where the current
  density is localized, corresponding to a resistively heated layer of
  plasma bounded by viscously heated plasma. The temperature gradient
  drives a thermoelectric current density that can have a magnitude
  greater than that of the electric-field-driven conduction current
  density, so thermoelectric effects are important in determining the
  Joule heating rate.

Title: Anisotropic transport processes in the chromosphere and
    overlying atmosphere
Authors: Goodman, M. L.; Kazeminezhad, F.
Bibcode: 2010MmSAI..81..631G
Altcode:
  Energy flow and transformation in the solar atmosphere is a complex
  process. Fluxes of particle kinetic and electromagnetic energy flow
  in both directions through the photosphere, and are transformed
  into one another in the overlying atmosphere. Diffusive transport
  processes such as electrical and thermal conduction, and viscous and
  thermoelectric effects play a major role in determining energy fluxes
  and transformation rates. Almost the entire atmosphere is strongly
  magnetized, meaning that charged particle cyclotron frequencies
  significantly exceed their collision frequencies. This causes transport
  processes to be anisotropic, so they must be described by tensors in
  MHD models. Only models that include the relevant transport tensors
  can reveal the processes that create and maintain the chromosphere,
  transition region, and corona because only such models can accurately
  describe energy flow and transformation. This paper outlines the
  importance of anisotropic transport processes in the atmosphere,
  especially of anisotropic electrical conduction in the weakly ionized,
  strongly magnetized chromosphere, and presents MHD model evidence
  that anisotropic electrical conduction plays a major role in shock
  wave and Alfvén wave heating in the chromosphere. It is proposed
  that magnetization induced resistivity increases with height from the
  photosphere, exceeds the Spitzer resistivity eta <SUB>S</SUB> near
  the height of the local temperature minimum, increases with height to
  orders of magnitude &gt; eta <SUB>S</SUB>, and causes proton Pedersen
  current dissipation to be a major source of chromospheric heating.

Title: Simulation of Magnetohydrodynamic Shock Wave Generation,
    Propagation, and Heating in the Photosphere and Chromosphere Using
    a Complete Electrical Conductivity Tensor
Authors: Goodman, Michael L.; Kazeminezhad, Farzad
Bibcode: 2010ApJ...708..268G
Altcode:
  An electrical conductivity tensor is used in a 1.5D magnetohydrodynamic
  (MHD) simulation to describe how MHD shock waves may form, propagate,
  and heat the photosphere and chromosphere by compression and resistive
  dissipation. The spatial resolution is 1 km. A train of six shock
  waves is generated by a sinusoidal magnetic field driver in the
  photosphere with a period T = 30 s, mean of 500 G, and variation
  of 250 G. The duration of the simulation is 200 s. Waves generated
  in the photosphere evolve into shock waves at a height z ~ 375 km
  above the photosphere. The transition of the atmosphere from weakly
  to strongly magnetized with increasing height causes the Pedersen
  resistivity η<SUB> P </SUB> to increase to ~2000 times the Spitzer
  resistivity. This transition occurs over a height range of a few hundred
  kilometers near the temperature minimum of the initial state at z ~
  500 km. The initial state is a model atmosphere derived by Fontenla
  et al., plus a background magnetic field. The increase in η<SUB>
  P </SUB> is associated with an increase in the resistive heating
  rate Q. Shock layer thicknesses are ~10-20 km. They are nonzero due
  to the presence of resistive dissipation, so magnetization-induced
  resistivity plays a role in determining shock structure, and hence the
  compressive heating rate Q<SUB>c</SUB> . At t = 200 s the solution has
  the following properties. Within shock layers, Q <SUB>maximum</SUB> ~
  1.4-7 erg cm<SUP>-3</SUP> s<SUP>-1</SUP>, and Q <SUB> c,maximum</SUB> ~
  10-10<SUP>3</SUP> Q <SUB>maximum</SUB>. Between shock waves, and at some
  points within shock layers, Q<SUB>c</SUB> &lt; 0, indicating cooling by
  rarefaction. The integrals of Q and Q<SUB>c</SUB> over the shock wave
  train are F ~ 4.6 × 10<SUP>6</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>
  and F<SUB>c</SUB> ~ 1.24 × 10<SUP>9</SUP> erg cm<SUP>-2</SUP>
  s<SUP>-1</SUP>. A method based on the thermal, mechanical, and
  electromagnetic energy conservation equations is presented for checking
  the accuracy of the numerical solution, and gaining insight into energy
  flow and transformation. The method can be applied to higher dimensional
  simulations. It is suggested that observations be performed to map out
  the transition region across which the transition from weakly ionized,
  weakly magnetized plasma to weakly ionized, strongly magnetized plasma
  occurs, and to correlate it with net radiative loss.

Title: Models for the Spectral Energy Distibution of Disks at Long
    Wavelengths
Authors: Goodman, Michael; Ignace, R.
Bibcode: 2010AAS...21542806G
Altcode: 2010BAAS...42R.345G
  We discuss the spectral energy distributions (SEDs) of axisymmetric
  circumstellar disks that produce infrared (IR), millimeter (mm),
  and radio emission excesses. In particular, we explore the effects of
  disk flaring on the SED shape. We find that relatively mild deviations
  from a power-law SED result from flaring. Key diagnostics for assessing
  flared disks from the SEDs are highlighted, and applications to IR and
  mm spectral measurements for Be star disks are noted. <P />This research
  was funded by a grant from the National Science Foundation, AST-0936427.

Title: MHD Model Estimates of the Contribution of Driven, Linear,
    Non-Plane Wave Dissipation to Chromospheric Heating Using a Complete
    Electrical Conductivity Tensor
Authors: Goodman, M. L.
Bibcode: 2008AGUFMSH51C..07G
Altcode:
  Analytic solutions of an MHD model that includes an anisotropic,
  inhomogeneous electrical conductivity tensor containing Hall, Pedersen,
  and Spitzer conductivities are used to compute resistive heating rates
  as a function of height z from the photosphere to the lower corona due
  to dissipation of driven, linear, non- plane waves. The background
  state of the atmosphere is assumed to be an FAL atmosphere. This
  state is linearly perturbed by a harmonic perturbation of frequency
  ν. The height dependence of the perturbation in the presence of
  the inhomogeneous background state is determined by solving the MHD
  equations given the harmonic, horizontal, driving magnetic field
  Bx1 at the photosphere, the constant vertical magnetic field Bz,
  and the magnetic field strength Bcond(z) that enters the electrical
  conductivity tensor. The variation of the heating rates per unit
  volume and mass with ν, Bx1, and Bcond(0) are determined. The
  heating rates are found to be ∝ Bcond(0)2 Bx12, and to increase with
  ν. The Pedersen resistivity is ∝ Bcond(0)2. It is several orders of
  magnitude greater than the Spitzer resistivity in the chromosphere, and
  determines the rate of heating by Pedersen current dissipation in the
  chromosphere. The Pedersen current is essentially a proton current in
  the chromosphere. The onset of Pedersen current dissipation rates large
  enough to balance the net radiative loss from the chromosphere occurs
  near the height of the FAL temperature minimum, and is triggered by
  the product of the electron and proton magnetizations first exceeding
  unity. The magnetizations and heating rate increase rapidly with
  height beginning near the temperature minimum. For the special case
  of Bz = 200 G, Bx1=140 G, and 400 ≤ Bcond(0) ≤ 1500 G the driver
  frequency for which the period averaged chromospheric heating flux
  FCh = 5 × 106 ergs-cm-2-sec-1 has the corresponding range of 91 ≥
  ν ≥ 25 mHz. Larger magnetic field strengths correspond to lower
  frequencies for a given heating rate. At magnetic field strengths
  &lt; 400 G, this value of FCh is achieved only at higher frequencies
  corresponding to solutions that violate the linear approximation. For
  the similar special case of Bz = 200 G, Bx1=140 G, and 50 ≤ Bcond(0)
  ≤ 1500 G the range of the maximum allowed driver frequency that is
  consistent with the linear approximation is 100.25 ≥ ν ≥ 92.5
  mHz. The corresponding range of FCh is 2 × 106 ≤ FCh ≤ 5.4 × 107
  ergs-cm-2-sec-1. This raises the possibility that linear MHD waves with
  periods ~ 10 seconds might make a major contribution to chromospheric
  heating in regions where the photospheric magnetic field strength is
  moderate to high. These results support the proposition of Goodman
  (e.g. Goodman 2000, ApJ, 533, 501; Goodman 2004, A&amp;A, 424, 691;
  Kazeminezhad &amp; Goodman 2006, ApJ, 166, 613) that the onset of
  electron and proton magnetization near the local temperature minimum,
  and their rapid increase with height causes the rate of proton Pedersen
  current dissipation to rapidly increase by orders of magnitude with
  height, creating and maintaining the solar chromosphere, and the
  chromospheres of solar type stars. This mechanism is not restricted to
  linear waves. It operates on any current generating MHD process. This
  work was supported by Grant ATM 0650443 from the National Science
  Foundation to the West Virginia High Technology Consortium Foundation.

Title: MHD Simulations of Shock Wave Generation, Propagation,
    and Heating in the Photosphere and Chromosphere Using a Complete
    Electrical Conductivity Tensor
Authors: Kazeminezhad, F.; Goodman, M. L.
Bibcode: 2008AGUFMSH41A1608K
Altcode:
  A complete anisotropic, inhomogeneous electrical conductivity tensor,
  which includes Spitzer, Pedersen, and Hall conductivities is included in
  an MHD simulation to describe how MHD shock waves may form, propagate,
  and resistively heat the atmosphere from the photosphere through the
  chromosphere. The MHD model includes an energy equation. The initial
  state is defined by FAL density, pressure, and temperature profiles, and
  by a magnetic field that decreases with height z. The initial magnetic
  field strength at the photosphere is 500 G. A harmonic magnetic field
  perturbation with amplitude 250 G and period 30 seconds is applied at
  the photosphere. Smooth waves are generated at the photosphere that
  propagate upward and begin to form shock waves near z=350 km. This
  is the height near which electrons first become magnetized. The
  shocks become fully formed near the FAL temperature minimum at z=500
  km. This is the height where the product of the electron and proton
  magnetizations first exceeds unity, causing the Pedersen resistivity to
  begin to rapidly exceed the Spitzer resistivity by orders of magnitude
  with increasing height. This is also the height at which heating by
  proton Pedersen current dissipation rapidly increases with height,
  and rapidly becomes large enough to balance the radiative losses from
  the chromosphere. The onset of this strong heating is triggered by
  the onset of electron and proton magnetization near the temperature
  minimum. The shock thicknesses are ~ ~ 5 km. The shocks are the sites
  of resistive heating rates as large as 3-10 ergs-cm-3-sec-1 in the
  chromosphere. The time averaged heating rate over an interval of
  162 seconds corresponds to a chromospheric heating flux ~ 2-3 × 106
  ergs-cm-2-sec-1. The heating rate increases with driving frequency,
  and is ∝ B2. These results support the proposition of Goodman
  (e.g. Goodman 2000, ApJ, 533, 501; Goodman 2004, A&amp;A, 424,691;
  Kazeminezhad &amp; Goodman 2006, ApJ, 166, 613) that the onset of
  electron and proton magnetization near the local temperature minimum,
  and their rapid increase with height causes the rate of proton Pedersen
  current dissipation to rapidly increase by orders of magnitude with
  height, creating and maintaining the solar chromosphere, and the
  chromospheres of solar type stars. This mechanism is not restricted to
  shock waves. It operates on any current generating MHD process. Such a
  process must involve currents driven by a combination of induction and
  convection generated electric fields. Examples are linear waves, and
  steady convection across magnetic field lines. It is the weakly ionized,
  strongly magnetized nature of the chromosphere that allows this heating
  mechanism to be so effective, and that distinguishes the chromosphere
  from the weakly ionized, weakly magnetized photosphere, and the strongly
  ionized, strongly magnetized corona. The dominance of proton-neutral H
  collisions in determining the proton collision frequency is necessary
  for this Pedersen current dissipation mechanism to be an effective
  heating mechanism in the chromosphere. This work was supported by Grant
  ATM 0650443 from the National Science Foundation to the West Virginia
  High Technology Consortium Foundation. <P />class="ab'&gt;

Title: Magnetohydrodynamic Simulations of Solar Chromospheric Dynamics
    Using a Complete Electrical Conductivity Tensor
Authors: Kazeminezhad, Farzad; Goodman, Michael L.
Bibcode: 2006ApJS..166..613K
Altcode:
  A 1.5-dimensional, time-dependent magnetohydrodynamic (MHD) model that
  includes an energy equation and anisotropic electrical conductivity
  tensor for a variably ionized, multispecies plasma is presented. The
  model includes an algorithm that reduces the numerical dissipation
  rate far below the dissipation rate determined by the conductivity
  tensor. This is necessary for accurate calculation of resistive heating
  rates. The model is used to simulate the propagation of Alfvén waves
  launched near the base of the middle chromosphere. The background
  state is the FAL CM equilibrium with a vertical magnetic field. The
  initial magnetic energy of a wave is almost completely damped out in
  the chromosphere by the time the disturbance propagates a distance of
  one wavelength. The energy is converted mainly into thermal energy. The
  remainder is converted into bulk flow kinetic energy and a Poynting
  flux with nonzero divergence. The thermal energy is generated almost
  entirely by Pedersen current dissipation. The corresponding heating
  rates are close to the FAL CM values near the base of the middle
  chromosphere. Dynamo action is observed. The damping of a continuously
  driven Alfvén wave train is also simulated, yielding results similar
  to those of the single wave cases. It is the strong magnetization and
  weak ionization of the chromosphere that allows for strong heating
  by Pedersen current dissipation. This distinguishes the chromosphere
  from the weakly magnetized and weakly ionized photosphere, and the
  strongly magnetized and strongly ionized corona where Pedersen current
  dissipation is not significant on the length and timescales simulated.

Title: Review of Particle Physics
Authors: Yao, W. -M.; Amsler, C.; Asner, D.; Barnett, R. M.; Beringer,
   J.; Burchat, P. R.; Carone, C. D.; Caso, C.; Dahl, O.; D'Ambrosio, G.;
   De Gouvea, A.; Doser, M.; Eidelman, S.; Feng, J. L.; Gherghetta, T.;
   Goodman, M.; Grab, C.; Groom, D. E.; Gurtu, A.; Hagiwara, K.; Hayes,
   K. G.; Hernández-Rey, J. J.; Hikasa, K.; Jawahery, H.; Kolda, C.;
   Kwon, Y.; Mangano, M. L.; Manohar, A. V.; Masoni, A.; Miquel, R.;
   Mönig, K.; Murayama, H.; Nakamura, K.; Navas, S.; Olive, K. A.;
   Pape, L.; Patrignani, C.; Piepke, A.; Punzi, G.; Raffelt, G.; Smith,
   J. G.; Tanabashi, M.; Terning, J.; Törnqvist, N. A.; sTrippe, T. G.;
   Vogel, P.; Watari, T.; Wohl, C. G.; Workman, R. L.; Zyla, P. A.;
   Armstrong, B.; Harper, G.; Lugovsky, V. S.; Schaffner, P.; Artuso,
   M.; Babu, K. S.; Band, H. R.; Barberio, E.; Battaglia, M.; Bichsel,
   H.; Biebel, O.; Bloch, P.; Blucher, E.; Cahn, R. N.; Casper, D.;
   Cattai, A.; Ceccucci, A.; Chakraborty, D.; Chivukula, R. S.; Cowan,
   G.; Damour, T.; DeGrand, T.; Desler, K.; Dobbs, M. A.; Drees, M.;
   Edwards, A.; Edwards, D. A.; Elvira, V. D.; Erler, J.; Ezhela, V. V.;
   Fetscher, W.; Fields, B. D.; Foster, B.; Froidevaux, D.; Gaisser,
   T. K.; Garren, L.; Gerber, H. -J.; Gerbier, G.; Gibbons, L.; Gilman,
   F. J.; Giudice, G. F.; Gritsan, A. V.; Grünewald, M.; Haber, H. E.;
   Hagmann, C.; Hinchliffe, I.; Höcker, A.; Igo-Kemenes, P.; JAckson,
   J. D.; Johnson, K. F.; Karlen, D.; Kayser, B.; Kirkby, D.; Klein,
   S. R.; Kleinknecht, K.; Knowles, I. G.; Kowalewski, R. V.; Kreitz, P.;
   Kursche, B.; Kuyanov, Yu. V.; Lahav, O.; Langacker, P.; Liddle, A.;
   Ligeti, Z.; Liss, T. M.; Littenberg, L.; Liu, J. C.; Lugovsky, K. S.;
   Lugovsky, s. B.; Mannel, T.; Manley, D. M.; Marciano, W. J.; Martin,
   A. D.; Milstead, D.; Narain, M.; Nason, P.; Nir, Y.; Peacock, J. A.;
   Prell, S. A.; Quadt, A.; Raby, S.; Ratcliff, B. N.; Razuvaev, E. A.;
   Renk, B.; Richardson, P.; Roesler, S.; Rolandi, G.; Ronan, M. T.;
   Rosenberg, L. J.; Sachrajda, C. T.; Sakai, Y.; Sarkar, S.; Schmitt,
   M.; Schneider, O.; Scott, D.; Sjöstrand, T.; Smoot, G. F.; Sokolsky,
   P.; Spanier, S.; Spieler, H.; Stahl, A.; Stanev, T.; Streitmatter,
   R. E.; Sumiyoshi, T.; Tkachenko, N. P.; Trilling, G. H.; Valencia, G.;
   van Bibber, K.; Vincter, M. G.; Ward, D. R.; Webber, B. R.; Wells,
   J. D.; Whalley, M.; Wolfenstsein, L.; Womersley, J.; Woody, C. L.;
   Yamamoto, A.; Zenin, O. V.; Zhang, J.; Zhu, R. -Y.
Bibcode: 2006JPhG...33....1Y
Altcode:
  This biennial Review summarizes much of particle physics. Using data
  from previous editions, plus 2633 new measurements from 689 papers,
  we list, evaluate, and average measured properties of gauge bosons,
  leptons, quarks, mesons, and baryons. We also summarize searches
  for hypothetical particles such as Higgs bosons, heavy neutrinos, and
  supersymmetric particles. All the particle properties and search limits
  are listed in Summary Tables. We also give numerous tables, figures,
  formulae, and reviews of topics such as the Standard Model, particle
  detectors, probability, and statistics. Among the 110 reviews are many
  that are new or heavily revised including those on CKM quark-mixing
  matrix, V<SUB>ud</SUB> &amp; V<SUB>us</SUB>, V<SUB>cb</SUB> &amp;
  V<SUB>ub</SUB>, top quark, muon anomalous magnetic moment, extra
  dimensions, particle detectors, cosmic background radiation, dark
  matter, cosmological parameters, and big bang cosmology. A booklet is
  available containing the Summary Tables and abbreviated versions of
  some of the other sections of this full Review. All tables, listings,
  and reviews (and errata) are also available on the Particle Data Group
  website: <A href="http://pdg.lbl.gov">http://pdg.lbl.gov</A>.

Title: MHD Simulations of Chromospheric Dynamics Using a Complete
    Electrical Conductivity Tensor
Authors: Kazeminezhad, Farzad; Goodman, M.
Bibcode: 2006SPD....37.0204K
Altcode: 2006BAAS...38R.221K
  A 1.5 D MHD simulation that includes an energy equation and a complete
  space and timedependent electrical conductivity tensor valid for
  a variably ionized plasma is used tostudy Alfven, magnetoacoustic,
  and acoustic wave propagation in the chromosphere. Heatingrates due
  to dissipation of magnetic field aligned and Pedersen currents are
  computed andcompared with FAL values. The model includes a numerical
  method that reduces the numerical dissipationrate far below the physical
  dissipation rate determined by the conductivity tensor. Wavelengths of
  80 - 220 km, and a spatial resolution of 10 km are used. The background
  state is the FAL equilibriumstate with a constant vertical magnetic
  field. For magnetic waves, the initial energy is converted intothermal
  energy, bulk flow kinetic energy, and a Poynting flux of energy
  with a non-zero divergence.It is verified that Poynting's theorem is
  satisfied. The waves are launched 10^3 km above the FAL photosphere. The
  magnetic waves are rapidly damped outnear this height, and produce
  heating rates close to the corresponding FAL value. It is the strong
  magnetization and weak ionization of the chromospherethat allows for
  the strong wave heating. This heating is duealmost entirely to Pedersen
  current dissipation.This distinguishes the chromospherefrom the weakly
  magnetized and weakly ionized photosphere, and the strongly magnetized
  and stronglyionized corona where Pedersen current dissipation is not
  a significant heating mechanism on the lengthand time scales simulated.

Title: Self-consistent Magnetohydrodynamic Modeling of Current Sheet
    Structure and Heating Using Realistic Descriptions of Transport
    Processes
Authors: Goodman, Michael L.
Bibcode: 2005ApJ...632.1168G
Altcode:
  A magnetohydrodynamic (MHD) model of an electron-ion,
  collision-dominated plasma that includes the electrical conductivity
  and thermoelectric tensors in Ohm's law is used to generate current
  sheet solutions in parameter ranges that correspond to those of
  the solar transition region and lower corona. The model contains
  a prescribed sheared magnetic field with a characteristic length
  scale L. The characteristic sheet width is 2L, but it is found that
  the temperature has transition region or coronal values only within
  a diffusion region (DR) with a width several orders of magnitude
  smaller than 2L. The heating rate per unit mass and flow speed in
  the DR are orders of magnitude larger, and the density is orders of
  magnitude smaller than in the surrounding plasma. The heating rate
  per unit volume is a maximum in the DR and falls off steadily outside
  the DR. The Joule heating rate and current density each consist of a
  conduction component driven by the center-of-mass electric field and
  a thermoelectric component driven by the temperature gradient. It is
  found that these components largely cancel, leading to a total heating
  rate and current density orders of magnitude smaller than either of
  their components. This suggests that thermoelectric current drive is
  important in determining current sheet structure. The center-of-mass
  electric field that provides the energy to maintain the plasma in a
  steady state is almost entirely the convection electric field. The
  electron magnetization M<SUB>e</SUB> is the product of the electron
  cyclotron frequency and the electron-ion collision time. Nonzero values
  of M<SUB>e</SUB> cause the conductivity and thermoelectric tensors to
  be anisotropic. It is found that the large values of M<SUB>e</SUB>
  that occur in the DR increase the heating rates per unit volume and
  mass by several orders of magnitude and can change the sign of the
  heating rate per unit mass from negative to positive, corresponding to
  a change from a cooling process to a heating process. This suggests
  that electron magnetization, and hence anisotropic transport, is a
  major factor in current sheet heating.

Title: Megaton Water Cerenkov Detectors and Astrophysical Neutrinos
Authors: Goodman, M.
Bibcode: 2005NuPhS.145..335G
Altcode: 2005astro.ph..1480G
  Although formal proposals have not yet been made, the UNO and
  Hyper-Kamiokande projects are being developed to follow-up the
  tremendously successful program at Super-Kamiokande using a detector
  that is 20-50 times larger. The potential of such a detector to continue
  the study of astrophysical neutrinos is considered and contrasted with
  the program for cubic kilometer neutrino observatories.

Title: Investigation of Solar Coronal Heating Using a Time Dependent
    MHD Model with Full Conductivity Tensor
Authors: Kazeminezhad, F.; Goodman, M. L.
Bibcode: 2005AGUSMSP41A..07K
Altcode:
  The transition region and lower corona is investigated using a newly
  developed time dependent MHD model that includes gravity and a self
  consistently computed conductivity tensor that depends on temperature,
  magnetic field, and density. The model is tested by its ability to
  preserve FAL equilibrium profiles, and to generate MHD waves with
  dispersion relations similar to those predicted by linear theory for
  the general types of MHD waves. The model is then used to examine
  solar atmospheric heating by Pedersen and magnetic field aligned
  current dissipation. Numerical experiments are conducted in which
  MHD waves are launched from either the transition region upward,
  or from the lower corona downward. Results from parametric studies
  of the evolution of these waves as a function of wavelength and
  amplitude are presented. In particular, the heating rate due to wave
  dissipation is compared with the FAL cooling rate, and with analytic
  results presented in M. Goodman [1,2]. % . The relative importance
  of physical dissipation due to the conductivity tensor, and numerical
  dissipation is estimated using Von Neumann stability analysis (VNSA)
  and numerical experiments with and without physical dissipation. It is
  then attempted to extrapolate from the simulation data the waves which
  could potentially lead to the correct heating rate, assumed to be the
  FAL net radiative loss rate. Realistic solar atmospheric data is used
  throughout the numerical investigations. This work was supported in
  part by NSF grant ATM-0242820 to the Institute for Scientific Research.

Title: Chromospheric Heating, Transport Processes, and Small Scale
    Magnetic Fields
Authors: Goodman, M. L.
Bibcode: 2005AGUSMSH11C..01G
Altcode:
  There are two basic categories of theories of chromospheric
  heating: hydrodynamic heating, and magnetohydrodynamic (MHD)
  heating. Hydrodynamic heating by shock wave dissipation appears
  to explain the origin of internetwork CaII bright points, but the
  associated heating rate appears to be at least one order of magnitude
  smaller than what is required to balance the chromospheric net radiative
  loss. Heating by high frequency acoustic waves is a proposed mechanism
  for chromospheric heating, at least in the internetwork, but so far
  there is no observational evidence that the energy in such waves is
  sufficient to heat the chromosphere. Increasing observational evidence
  for the existence of magnetic field concentrations at or below the
  spatial resolution limit with strengths ~ 102 - 103 G, the positive
  correlation between magnetic field strength and net radiative loss,
  and the differences between network, internetwork, and active regions
  in terms of magnetic field filling factor and net radiative loss suggest
  that a single MHD mechanism heats the network, internetwork, and active
  region chromospheres outside of flaring regions, and operates largely at
  or below the spatial resolution limit. A discussion of this suggestion
  in the context of the critical need to model proposed chromospheric
  heating mechanisms using realistic transport processes is presented
  along with an indication of why this heating mechanism is not effective
  in the transition region or corona, except possibly on spatial scales
  believed to characterize current sheets. This work was supported by
  NSF grant ATM-0242820 to the Institute for Scientific Research.

Title: Self Consistent Modeling of Current Sheet Structure and
    Transport Processes
Authors: Goodman, M. L.
Bibcode: 2005AGUSMSP22A..05G
Altcode:
  A simple magnetohydrodynamic (MHD) model of a fully ionized,
  collision dominated plasma that includes the electrical conductivity
  and thermoelectric tensors in Ohm's law is used to generate current
  sheet solutions that, where the assumption of full ionization is valid,
  are characterized by ranges of temperature, density, magnetic field
  strength, and flow speed that correspond to those of the transition
  region and corona. The electrical conductivity and thermoelectric
  tensors are functions of temperature, number density, and magnetic
  field strength. The model contains a prescribed sheared magnetic field
  with a characteristic length scale L. The characteristic sheet width
  is 2L, but the temperature has transition region or coronal values
  only within a central plasma sheet (CPS) that has a width one or
  more orders of magnitude smaller than 2L. The CPS is essentially the
  diffusion region. The heating rate per unit mass, and the flow speed
  in the CPS are orders of magnitude larger, and the density is orders of
  magnitude smaller than in the surrounding plasma. The heating rate per
  unit volume is a maximum in the CPS, and falls off steadily outside
  the CPS. The heating is driven almost entirely by the convection
  electric field. The current density and heating rate each consist of
  a thermoelectric component driven by the temperature gradient, and a
  conduction component driven by the center of mass electric field. These
  components largely cancel one another, yielding a total current density
  and heating rate that are orders of magnitude smaller than either
  of their components. This suggests that thermoelectric effects are
  important in determing current sheet structure. This work was supported
  by NSF grant ATM-0242820 to the Institute for Scientific Research.

Title: On the creation of the chromospheres of solar type stars
Authors: Goodman, M. L.
Bibcode: 2004A&A...424..691G
Altcode:
  A mechanism that creates the chromospheres of solar type stars
  everywhere outside of flaring regions is proposed. The identification
  of the mechanism is based on previous work and on the results of a
  model presented here that computes the electric current, its driving
  electric field, the heating rate due to resistive dissipation, and
  the flow velocity in a specified class of horizontally localized, two
  dimensional magnetic structures in the steady state approximation. The
  model is applied to the Sun over the height range from the photosphere
  to the upper chromosphere. Although the model does not contain time
  explicitly, it contains information about the dynamics of the atmosphere
  through inputs from the FAL CM solar atmosphere model, which is based on
  time averages of spectroscopic data. The model is proposed to describe
  the time averaged properties of the heating mechanism that creates the
  chromosphere. The model magnetic structure is horizontally localized,
  but describes heating of the global chromosphere in the following
  way. Recent observations indicate that kilogauss strength magnetic
  structures exist in the photospheric internetwork with a filling
  factor f∼ 2%, and characteristic diameters &lt; 180 km. Assuming f
  = 2 % and a maximum field strength of 10<SUP>3</SUP> G for the model
  magnetic structure, and assuming that the chromospheric heating rate
  predicted by FAL CM represents a horizontal spatial average over such
  magnetic structures, it is found that the model magnetic structures that
  best reproduce the FAL CM heating rate as a function of height have
  characteristic diameters in the range of 98 - 161 km, consistent with
  the upper bound inferred from observation. Based on model solutions
  and previous work it is proposed that essentially all chromospheric
  heating occurs in magnetic structures with sub-resolution horizontal
  spatial scales (⪉ 150 ; km), that the heating is due to dissipation of
  Pedersen currents driven by a convection electric field, and that it is
  the increase in the magnetization of particles with height in a magnetic
  structure from values ≪1 in the lower photosphere to values ⪆1 near
  the height of the temperature minimum in the magnetic structure that
  causes the Pedersen current dissipation rate to increase to a value
  large enough to cause a temperature inversion. The magnetization of a
  particle is the ratio of its cyclotron frequency to its total collision
  frequency with unlike particle species.

Title: Review of Particle Physics
Authors: Particle Data Group; Eidelman, S.; Hayes, K. G.; Olive, K. A.;
   Aguilar-Benitez, M.; Amsler, C.; Asner, D.; Babu, K. S.; Barnett,
   R. M.; Beringer, J.; Burchat, P. R.; Carone, C. D.; Caso, S.; Conforto,
   G.; Dahl, O.; D'Ambrosio, G.; Doser, M.; Feng, J. L.; Gherghetta, T.;
   Gibbons, L.; Goodman, M.; Grab, C.; Groom, D. E.; Gurtu, A.; Hagiwara,
   K.; Hernández-Rey, J. J.; Hikasa, K.; Honscheid, K.; Jawahery, H.;
   Kolda, C.; Kwon, Y.; Mangano, M. L.; Manohar, A. V.; March-Russell,
   J.; Masoni, A.; Miquel, R.; Mönig, K.; Murayama, H.; Nakamura, K.;
   Navas, S.; Pape, L.; Patrignani, C.; Piepke, A.; Raffelt, G.; Roos, M.;
   Tanabashi, M.; Terning, J.; Törnqvist, N. A.; Trippe, T. G.; Vogel,
   P.; Wohl, C. G.; Workman, R. L.; Yao, W. -M.; Zyla, P. A.; Armstrong,
   B.; Gee, P. S.; Harper, G.; Lugovsky, K. S.; Lugovsky, S. B.; Lugovsky,
   V. S.; Rom, A.; Artuso, M.; Barberio, E.; Battaglia, M.; Bichsel, H.;
   Biebel, O.; Bloch, P.; Cahn, R. N.; Casper, D.; Cattai, A.; Chivukula,
   R. S.; Cowan, G.; Damour, T.; Desler, K.; Dobbs, M. A.; Drees, M.;
   Edwards, A.; Edwards, D. A.; Elvira, V. D.; Erler, J.; Ezhela, V. V.;
   Fetscher, W.; Fields, B. D.; Foster, B.; Froidevaux, D.; Fukugita,
   M.; Gaisser, T. K.; Garren, L.; Gerber, H. -J.; Gerbier, G.; Gilman,
   F. J.; Haber, H. E.; Hagmann, C.; Hewett, J.; Hinchliffe, I.; Hogan,
   C. J.; Höhler, G.; Igo-Kemenes, P.; Jackson, J. D.; Johnson, K. F.;
   Karlen, D.; Kayser, B.; Kirkby, D.; Klein, S. R.; Kleinknecht, K.;
   Knowles, I. G.; Kreitz, P.; Kuyanov, Yu. V.; Lahav, O.; Langacker,
   P.; Liddle, A.; Littenberg, L.; Manley, D. M.; Martin, A. D.;
   Narain, M.; Nason, P.; Nir, Y.; Peacock, J. A.; Quinn, H. R.; Raby,
   S.; Ratcliff, B. N.; Razuvaev, E. A.; Renk, B.; Rolandi, G.; Ronan,
   M. T.; Rosenberg, L. J.; Sachrajda, C. T.; Sakai, Y.; Sanda, A. I.;
   Sarkar, S.; Schmitt, M.; Schneider, O.; Scott, D.; Seligman, W. G.;
   Shaevitz, M. H.; Sjöstrand, T.; Smoot, G. F.; Spanier, S.; Spieler,
   H.; Spooner, N. J. C.; Srednicki, M.; Stahl, A.; Stanev, T.; Suzuki,
   M.; Tkachenko, N. P.; Trilling, G. H.; Valencia, G.; van Bibber, K.;
   Vincter, M. G.; Ward, D. R.; Webber, B. R.; Whalley, M.; Wolfenstein,
   L.; Womersley, J.; Woody, C. L.; Zenin, O. V.; Zhu, R. -Y.
Bibcode: 2004PhLB..592....1P
Altcode: 2004PhLB..592....1E
  No abstract at ADS

Title: On the Creation of the Chromospheres of Solar Type Stars
Authors: Goodman, M. L.
Bibcode: 2004AAS...204.2904G
Altcode: 2004BAAS...36..695G
  A mechanism that creates the chromospheres of solar type stars
  everywhere outside of flaring regions is presented. The identification
  of the mechanism is based on previous work and on the results of a
  model presented here that computes the flow velocity, electric current,
  its driving electric field, and the heating rate due to resistive
  dissipation in a specified class of horizontally localized, two
  dimensional magnetic structures in the steady state approximation. The
  model is applied to the Sun over the height range from the photosphere
  to the upper chromosphere. Although the model does not contain time
  explicitly, it contains information about the dynamics of the atmosphere
  through inputs from the FAL CM solar atmosphere model, which is based on
  time averages of spectroscopic data. The model is proposed to describe
  the time averaged properties of the heating mechanism that creates the
  chromosphere. The model predicts that essentially all chromospheric
  heating occurs in magnetic structures with sub-resolution horizontal
  spatial scales, that the heating is due to dissipation of Pedersen
  currents driven by a convection electric field, and that it is the
  increase in the magnetization of particles with height in a magnetic
  structure from values &lt;&lt; 1 in the lower photosphere to values ≳
  1 near the height of the temperature minimum in the magnetic structure
  that causes the Pedersen current dissipation rate to increase to a value
  large enough to cause a temperature inversion. The magnetization of a
  particle is the ratio of its cyclotron frequency to its total collision
  frequency with unlike particle species. The model magnetic structure is
  horizontally localized, but is used to describe heating of the global
  chromosphere in the following way. Recent observations indicate that
  kilogauss strength magnetic structures exist in the photospheric
  internetwork with a filling factor f ∼ 2 %, and characteristic
  diameters &lt; 180 km. Assuming f = 2 % and a maximum field strength of
  10<SUP>3</SUP> G for the model magnetic structure, and assuming that the
  chromospheric heating rate predicted by FAL CM represents a horizontal
  spatial average over such magnetic structures, it is found that the
  model magnetic structures that best reproduce the FAL CM heating rate
  as a function of height have characteristic diameters in the range of
  98 - 161 km, consistent with the upper bound inferred from observation.

Title: On the efficiency of plasma heating by Pedersen current
    dissipation from the photosphere to the lower corona
Authors: Goodman, M. L.
Bibcode: 2004A&A...416.1159G
Altcode:
  A model is presented that uses the electrical conductivity tensor of
  a multi-species plasma to estimate the efficiency Q of plasma heating
  by Pedersen current dissipation as a function of height from the
  photosphere to the lower corona. The particle densities and temperature
  are given by FAL model CM. Q is the efficiency with which the electric
  field generates thermal energy by transferring energy to the current
  density J<SUB>⊥</SUB> perpendicular to the magnetic field. The energy
  is then thermalized by collisions. The projection of J<SUB>⊥</SUB>
  on the driving electric field is the Pedersen current density. Q
  is the ratio of the actual heating rate due to Pedersen current
  dissipation to the heating rate when J<SUB>⊥</SUB> is entirely a
  Pedersen current, which is the maximum possible heating rate for given
  J<SUB>⊥</SUB>. It is found that Pedersen current dissipation is highly
  efficient throughout the chromosphere, but is highly inefficient in the
  transition region and corona on the spatial scales of FAL CM. In the
  photosphere, the electron magnetization, which is the product of the
  cyclotron frequency and the collision time is so small compared to unity
  that the conductivity tensor is almost isotropic, implying there is no
  essential difference between Pedersen current dissipation and magnetic
  field aligned current dissipation. It is the rapid increase with height
  of the magnetizations of electrons, protons and metallic ions from
  ≲ 1 to ≫ 1 beginning near the height of the FAL CM temperature
  minimum that causes Pedersen current dissipation to become essentially
  different from magnetic field aligned current dissipation, and that
  causes Q to rapidly increase from minimum values ∼ 0.1 near the
  temperature minimum to ∼ 1 in the lower chromosphere. Q remains ∼
  1 up to the transition region in which it precipitously decreases with
  height to values ≲ 10<SUP>-10</SUP> in the corona. It is proposed that
  the rapidly increasing magnetization triggers the onset of heating by
  Pedersen current dissipation that causes the chromospheric temperature
  inversion and heats the entire non-flaring chromosphere. The energy
  channeled by any mechanism into the generation of a center of mass
  (CM) electric field that drives current perpendicular to the magnetic
  field is thermalized by Pedersen current dissipation at the maximum
  possible rate throughout the chromosphere. The mechanism is damped
  in the chromosphere to the degree to which its energy is channeled
  into the creation of the CM electric field. The results of the model
  are consistent with previous predictions that slow magnetoacoustic
  waves heat network regions of the chromosphere through dissipation
  of Pedersen currents driven by a wave generated convection electric
  field, and that electric current dissipation on the spatial scales of
  the FAL models is insignificant for heating the transition region.

Title: Physical Modeling of the Solar Radiation, Current Status
    and Prospects
Authors: Fontenla, J. M.; Avrett, E. H.; Goodman, M.; White, O. W.;
   Rottman, G.; Fox, P.; Harder, J.
Bibcode: 2003SPD....34.0301F
Altcode: 2003BAAS...35..808F
  Physical models that include full NLTE radiative transfer as well as
  particle transport and MHD processes are the key to understanding the
  solar radiative output and also are essential to our understanding
  of heating and the dynamics of the solar atmosphere, in particular
  for chromospheric layers. SOHO observations show that chromospheric
  emission lines do not vary dramatically in time and that chromospheric
  heating, even in the quiet Sun, is not simply due to, p-modes induced,
  strong shock waves passing through the chromosphere. The physics of
  the chromospheric heating is more complicated and remains elusive. The
  chromospheric and coronal heating are likely closely related to the
  dynamics in these regions as well as in the thin chromosphere-corona
  transition region since they are a coupled system. Solar atmospheric
  heating and dynamics are strongly affected by the magnetic fields and
  MHD mechanisms must be considered. Models for the upper photosphere
  and chromosphere should also consider NLTE radiative transfer and
  radiative losses as well as particle transport processes including
  tensor electric resistivity with magnetic field. Models for the
  transition region and coronal layers must also consider particle
  diffusion. In this paper we show schematically: 1) the current state
  of our research on modeling observed features of the solar structure
  and their radiative signatures; 2) the application of this modeling
  to the Earth solar irradiance and comparisons with observations; 3)
  the key achievements and the needed improvements of the modeling; 4)
  our plans for future research starting from ab initio semi-empirical
  models based on observations, and, while maintaining the agreement with
  relevant observations, moving towards physically consistent models that
  include key MHD processes thereby replacing empirical constraints by
  physically consistent processes and boundary conditions.

Title: Predictions of Heating Rates in Localized Magnetic Structures
    From The Photosphere To The Upper Chromosphere
Authors: Goodman, M. L.
Bibcode: 2003SPD....34.1105G
Altcode: 2003BAAS...35R.827G
  The heating rates due to resistive dissipation of magnetic field
  aligned currents and of Pedersen currents are computed as functions
  of height and horizontal radius in a specified 2.5 D magnetic field
  from the photosphere to the upper chromosphere. The model uses the
  VAL C height dependent profiles of temperature, and electron, proton,
  hydrogen, helium, and heavy ion densities together with the magnetic
  field to compute the anisotropic electrical conductivity tensor for each
  charged particle species. The magnetic field is parameterized by its
  maximum magnitude B<SUB>0</SUB>, scale height L, characteristic diameter
  D<SUB>0</SUB>, and twist τ which is the ratio of the azimuthal field
  component to the radial field component. The objective is to determine
  the ranges of values of these parameters that yield heating rates that
  are within observational constraints for values of D<SUB>0</SUB> that
  are above and below the resolution limit of ∼ 150 km. This provides
  a test of the proposition that Pedersen current dissipation is a major
  source of chromopsheric heating in magnetic structures throughout the
  chromosphere, and that it is the rapid increase of charged particle
  magnetization with height in the lower chromosphere that causes the
  chromospheric temperature inversion and the rapid increase of the
  heating rate per unit mass with height in this region. It is found
  that the heating rate is a monotonically increasing function of
  B<SUB>0,</SUB> L, and τ , and a monotonically decreasing function
  of D<SUB>0</SUB>. For values of D<SUB>0</SUB> below the resolution
  limit, values of τ &gt;&gt; 1 correspond to strongly heated magnetic
  structures. <P />This work was supported by NSF grant ATM 9816335.

Title: Overview of Future Neutrino Experiments
Authors: Goodman, M.
Bibcode: 2003psc..confE..66G
Altcode:
  No abstract at ADS

Title: Plasma Heating by Pedersen Current Dissipation From the
    Photosphere to the Upper Chromosphere
Authors: Goodman, M. L.
Bibcode: 2002AGUFMSH52A0477G
Altcode:
  An MHD model is used to estimate the contribution of Pedersen
  current dissipation, as a function of height z, to plasma heating
  from the photosphere to the upper chromosphere. The model computes the
  particle diffusion velocities, normalized to the local drift velocity,
  transverse to a vertical magnetic field for a seven species plasma of
  electrons, protons, a proxy heavy ion, HeI, HeII, HeIII, and H. The
  proxy heavy ion is a single species representation of singly ionized C,
  Si, Al, Mg, Fe, Na, and Ca. The temperature and particle densities as
  functions of z are given by VAL model C. Collisions between all unlike
  particle species are taken into account. The diffusion velocities are
  used to compute the heating rate per unit volume Q(z), normalized
  to the maximum possible heating rate per unit volume at height z,
  due to Pedersen current dissipation. Q is the fraction of energy
  in the current density perpendicular to the magnetic field that
  is dissipated by collisions. Solutions to the model suggest that:
  (i) The solar chromosphere above photospheric magnetic fields with
  strengths ~ 10<SUP>2</SUP> - 10<SUP>3</SUP> G is heated by Pedersen
  current dissipation; (ii) This heating mechanism first becomes
  effective at heights corresponding to the lower chromosphere as
  defined by VAL; (iii) It is the rapid increase of charged particle
  magnetization with height in the lower chromosphere that triggers
  the rapid onset of intense heating by Pedersen current dissipation,
  where the magnetization is the ratio of the cyclotron frequency to the
  total collision frequency with unlike particles; (iv) Q(z) rapidly
  decreases to zero for z &gt; ~ 2100 km due to strong magnetization
  transforming the current perpendicular to the magnetic field into a
  Hall current, which is not dissipative; (v) The protons and the proxy
  heavy ions carry essentially all of the Pedersen current. These results
  suggest that network and internetwork regions of the chromosphere are
  heated by Pedersen current dissipation. The model does not assume or
  predict any form for the mechanism that drives the heating. However,
  the results of the model are consistent with previous predictions that
  magnetoacoustic waves heat network regions of the chromosphere through
  Pedersen current dissipation driven by a wave generated convection
  electric field. It is proposed that this wave heating mechanism also
  makes a major contribution to heating internetwork regions of the
  chromosphere. This work was supported by National Science Foundation
  grant ATM 9816335.

Title: Atmospheric Neutrinos in Soudan 2
Authors: Goodman, M.; Soudan 2 Collaboration
Bibcode: 2001ICRC....3.1085G
Altcode: 2001ICRC...27.1085G
  Neutrino interactions recorded in a 5.1 fiducial kiloton-year exposure
  of the Soudan-2 iron tracking calorimeter are analyzed for effects of
  neutrino oscillations. Using contained single track and single shower
  events, we update our measurement of the atmospheric / ratio-of-ratios
  and find . Assuming this anomalously low R-value is the result of
  flavor disappearance viat o oscillation, we select samples of charged
  current events which offer good resolution, event-by-event, for Ä
  reconstruction. Oscillation-weighted Monte Carlo events are fitted
  to these data events using a ¾ function summed over bins of log´Ä
  µ. The region allowed in the (× Ò¾ ¾ , ¡Ñ¾) plane at 90% CL is
  obtained using the Feldman-Cousins procedure: 1 DETECTOR; DATA EXPOSURE
  The Soudan-2 experiment will soon (July 2001) be completing the taking
  of data using its fine-grained iron tracking calorimeter of total mass
  963 tons. This detector images nonrelativistic as well as relativistic
  charged particles produced in atmospheric neutrino reactions. It
  has operated underground at a depth of 2100 meters-water-equivalent
  on level 27 of the Soudan Mine State Park in northern Minnesota. The
  calorimeter's modular design enabled data-taking to commence in April
  1989 when the detector was one quarter of its full size; assembly of
  the detector was completed during 1993. Data-taking continued with 85%
  live time, even though dynamite blasting has been underway nearby for
  the MINOS cavern excavation since Summer 1999. The total data exposure
  will be 5.8fiducial kiloton-years (kTy). Results presented here are
  based upon a 5.1 kTy exposure. The tracking calorimeter operates as a
  slow-drift (0.6 cm/ s) time projection chamber. Its tracking elements
  are meterlong plastic drift tubes which are placed into the corruga-

Title: Search for Nucleon Decay and n-nbar Oscillation in Soudan 2
Authors: Chung, J.; Fields, T.; Goodman, M.
Bibcode: 2001ICRC....4.1463C
Altcode: 2001ICRC...27.1463C
  We have studied multiprong contained events in the Soudan 2 detector
  in order to search for nucleon decay and neutron oscillation (and
  subsequent annihilation) into high multiplicity final states. The
  excellent spatial resolution of the Soudan 2 tracking calorimeter
  detector, together with its capability to identify slow proton tracks
  and stopping tracks through their higher ionization, enables us to
  analyze high multiplicity events in more detail than has been done
  previously. We have found no evidence for signal events above the
  (small) estimated backgroundof multiprong events due to atmospheric
  neutrino interactions.

Title: Horizontal Muons in Soudan 2 and Search for AGN Neutrinos
Authors: Demuth, D.; Goodman, M.
Bibcode: 2001ICRC....3.1089D
Altcode: 2001ICRC...27.1089D
  Using horizontal muons in Soudan 2, we measure the neutrino induced muon
  flux and set a limit on the flux of neutrinos from AGN's. A horizontal
  neutrino induced flux of 5.00 ± 0.55 ± 0.51 ×10-13 cm-2 sr-1 s-1
  is measured. The absence of horizontal muons with a large energy loss
  is used to set a limit on the flux of ν's from AGN's as a function
  of energy.

Title: The Necessity of Using Realistic Descriptions of Transport
    Processes in Modeling the Solar Atmosphere, and the Importance of
    Understanding Chromospheric Heating*
Authors: Goodman, Michael L.
Bibcode: 2001SSRv...95...79G
Altcode:
  Three points and research directions are discussed: The outstanding
  problem of identifying the mechanisms of solar atmospheric heating
  and wind acceleration can be solved only by combining quantitative
  models that include realistic descriptions of relevant transport
  processes with observational constraints on the inputs and outputs
  of these models. Most solar atmospheric heating, with the possible
  exception of flares, takes place in the chromosphere, emphasizing the
  importance of identifying the mechanisms of chromospheric heating,
  which may be important for understanding coronal heating and wind
  acceleration. Recent modeling leads to the conclusion that the onset
  of proton magnetization with increasing height in thin magnetic flux
  tubes triggers the onset of chromospheric network heating by resistive
  dissipation of Pedersen currents driven by the convection electric
  field of slow, longitudinal magnetoacoustic waves.

Title: Proton Magnetization as the Triggering Mechanism for
    Chromospheric Network Heating by Pedersen Current Dissipation
Authors: Goodman, M. L.
Bibcode: 2000SPD....31.0140G
Altcode: 2000BAAS...32..808G
  In thin magnetic flux tubes in the photospheric and lower chromospheric
  network, the product ω τ of the proton cyclotron frequency with
  the proton-hydrogen collision time increases with height. Near the
  photosphere (ω τ )<SUP>2</SUP> &lt;&lt; 1 in strong magnetic flux
  tubes. Near the height of the temperature minimum, which is different
  for flux tubes with different photospheric field strengths, (ω τ
  )<SUP>2</SUP> ~ 1. When (ω τ )<SUP>2</SUP> increases through unity
  the protons are said to become magnetized: at this height control
  of the proton dynamics switches from collisions with hydrogen to the
  magnetic field. This causes a rapid increase in the rate of Pedersen
  current dissipation, determined by the rapid change in the anisotropic
  conductivity tensor for a weakly ionized plasma of hydrogen, electrons,
  protons, and singly ionized heavy ions. The rapid increase of heating
  rate with height just above the temperature minimum in a flux tube
  is due to the continuing increase of proton magnetization with
  height, and to the following feedback mechanism: heating by Pedersen
  current dissipation ---&gt; increase in hydrogen ionization ---&gt;
  increase in ratio of proton number density to heavy ion number density
  ---&gt; increase in heating by Pedersen current dissipation. Above
  the temperature minimum the heating rate increases by one order of
  magnitude over one pressure scale height. The classical concept of
  a single temperature minimum about 500 km above the photosphere is
  interpreted as an average over the heights of the different temperature
  minima of different flux tubes. Ranges of hydrogen density and magnetic
  field strength for the lower chromospheric network are predicted. The
  current density is driven by slow, longitudinal, magnetoacoustic
  waves that have their source in the dynamic interaction between the
  photospheric granulation and the magnetic flux tubes concentrated at
  the granulation boundaries. The author gratefully acknowledges support
  by NSF grant ATM-9816335 to the Catholic University of America.

Title: On the Mechanism of Chromospheric Network Heating and the
    Condition for Its Onset in the Sun and Other Solar-Type Stars
Authors: Goodman, Michael L.
Bibcode: 2000ApJ...533..501G
Altcode:
  A mechanism for chromospheric network heating and a necessary and
  sufficient condition for its onset are presented. The heating
  mechanism consists of resistive dissipation of proton Pedersen
  currents, which flow orthogonal to the magnetic field in weakly
  ionized chromospheric plasma. The currents are driven by a convection
  electric field generated by velocity oscillations of linear, slow,
  longitudinal magnetoacoustic waves with frequencies ν&lt;~3.5 mHz
  in the lower chromosphere. The heating occurs in thin magnetic flux
  tubes and begins lower in the chromosphere in flux tubes with higher
  photospheric field strength. The lower chromosphere, which emits most
  of the net radiative loss in the network, is heated by flux tubes with
  photospheric field strengths ~700-1500 G. A typical field strength and
  core diameter for a flux tube in the lower chromosphere with a core
  heating rate of 10<SUP>7</SUP> ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>
  are 170 G and 10 km. This core region is contained in a region with
  a diameter ~100 km in which the heating rate is an order of magnitude
  smaller. About N~10<SUP>2</SUP> of these flux tubes distributed over
  the boundary region of a granule with a diameter ~10<SUP>3</SUP> km
  provide an average heating rate over the entire granule ~10<SUP>7</SUP>
  ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>. If the core heating rate is
  changed by a factor f, then N~f<SUP>-1/2</SUP>10<SUP>2</SUP>. The
  condition for the onset of heating is that the ratio of the proton
  cyclotron frequency to the proton-hydrogen collision frequency equal
  unity. This ratio increases with height, and the condition is satisfied
  at a single height in a given flux tube. At this height, control of the
  proton dynamics begins to be dominated by the magnetic field rather
  than by collisions with hydrogen, and the anisotropic nature of the
  electrical conductivity begins to play a critical role in resistive
  dissipation. The protons become magnetized. Heating by dissipation of
  heavy ion and, to a lesser extent, proton Pedersen currents causes
  the temperature to start increasing. The heating increases hydrogen
  ionization. With increasing height, and hence proton magnetization,
  the Pedersen current density rapidly increases with hydrogen ionization
  via positive feedback, and the proton number density rapidly reaches
  and exceeds the heavy ion number density, resulting in an increase
  in heating rate by an order of magnitude over only 1 pressure scale
  height. During this process the protons rapidly dominate the Pedersen
  current. Heating by dissipation of magnetic field aligned currents is
  insignificant. Below the height in the atmosphere at which the onset
  condition is satisfied, any current orthogonal to the magnetic field
  must be primarily a Hall current, which is nondissipative. Heating by
  this mechanism must occur to some degree in the chromospheric network
  of all solar-type stars. It is proposed to be the dominant mechanism of
  chromospheric network heating, although viscous dissipation may also be
  important if the core heating rate is much larger than ~10<SUP>7</SUP>
  ergs cm<SUP>-2</SUP> s<SUP>-1</SUP> or if the linear MHD waves studied
  here evolve into shock waves with increasing height. Flux tubes in the
  quiet chromosphere are predicted to have two possible core diameters:
  ~10 km, corresponding to flux tubes in which network heating occurs,
  and ~10<SUP>4</SUP>-10<SUP>5</SUP> km, perhaps corresponding to flux
  tubes in which active region heating might occur. The model has a
  singularity at the acoustic cutoff frequency, corresponding to periods
  near 3 minutes. Therefore, unless nonresistive damping mechanisms such
  as viscous dissipation and thermal conduction provide sufficiently
  strong damping, MHD oscillations with periods near 3 minutes in
  chromospheric magnetic flux tubes must be nonlinear.

Title: On the Mechanism of Chromospheric Network Heating, and the
    Condition for its Onset in the Sun and Other Solar Type Stars
Authors: Goodman, M. L.
Bibcode: 1999AAS...194.2307G
Altcode: 1999BAAS...31..861G
  A mechanism for chromospheric network heating, and a necessary and
  sufficient condition for its onset are presented. The heating mechanism
  consists of resistive dissipation of proton Pedersen currents, which
  flow orthogonal to the magnetic field in weakly ionized chromospheric
  plasma. The currents are driven by a convection electric field generated
  by velocity oscillations of linear magnetoacoustic waves with periods
  greater than about 5 minutes. Heating occurs in thin magnetic flux
  tubes, and begins lower in the chromosphere in flux tubes with higher
  photospheric field strength. The lower chromosphere, which emits most of
  the chromospheric radiation, is heated by flux tubes with photospheric
  field strengths in the range of 700 - 1500 G. A typical diameter and
  field strength for a heated flux tube in the lower chromosphere are 10
  km and 100 G. The condition for the onset of this heating mechanism
  is that the proton cyclotron frequency equal the proton-hydrogen
  collision frequency. When this occurs, heating by dissipation of
  heavy ion Pedersen currents begins to raise the gas temperature, and
  hydrogen ionization increases exponentially with temperature according
  to the Saha equation. The Pedersen current density rapidly increases
  as the proton number density rapidly reaches and exceeds the heavy
  ion number density, resulting in an increase in heating rate by an
  order of magnitude over a height increase of only one pressure scale
  height. During this process the protons rapidly dominate the Pedersen
  current. This heating mechanism and condition for its onset apply
  to all solar type stars: stars with a convection zone and associated
  dynamo action causing the formation of photospheric convection cells
  with strong magnetic field concentrations at their boundaries.

Title: Quantitative Magnetohydrodynamic Modeling of the Solar
    Transition Region
Authors: Goodman, Michael L.
Bibcode: 1998ApJ...503..938G
Altcode:
  The transition region (TR) is assumed to be a collision-dominated
  plasma. The dissipation and transport of energy in such a plasma
  is accurately described by the classical transport coefficients,
  which include the electrical and thermal conductivity, viscosity,
  and thermoelectric tensors. These tensors are anisotropic and are
  functions of local values of temperature, density, and magnetic field
  strength. The transport coefficients are valid for all magnetic
  field strengths and so may be used to study the physics of weakly
  as well as strongly magnetized regions of the TR. They may be used
  in an MHD model to obtain a self-consistent, realistic description
  of the TR. The physics of kinetic processes is included in the MHD
  model through the transport coefficients. As a first step in studying
  heating and cooling processes in the TR in a realistic, quantitative
  manner, a 1.5 dimensional, steady state MHD model with a specified
  temperature profile is developed. The momentum equation includes
  the inertial, pressure, magnetic, and gravitational forces. Ohm's
  law includes the exact expressions for the electrical conductivity
  and thermoelectric tensors. It is found that the contribution of the
  dissipation of large-scale electric currents to in situ heating of
  the TR is negligible, but that thermal energy flowing into the TR
  from the corona can provide the energy required to heat the TR. The
  possibility that significant in situ heating of the TR takes place
  through viscous dissipation or small-scale electric current dissipation
  such as may occur in current sheets or filaments is discussed, although
  these processes are not described by the model. The importance of
  thermoelectric and electron pressure gradient effects in Ohm's law,
  and in determining the electron heat flux, is demonstrated. Results of
  the model suggest that the force-free approximation is not valid over
  most of the TR. Justification for assuming that the TR is collision
  dominated is presented. In particular, a self-consistent calculation
  of the ratio of the electric field parallel to the magnetic field to
  the Dreicer electric field yields a value &lt;~10<SUP>-3</SUP>, which
  suggests that anomalous transport processes are not important. The
  necessity of using a realistic description of transport processes in
  modeling heating mechanisms in the solar atmosphere is stressed.

Title: Convection driven heating of the solar middle chromosphere
    by resistive dissipation of large scale electric currents. II.
Authors: Goodman, M. L.
Bibcode: 1997A&A...325..341G
Altcode:
  A generalization of a recently developed MHD model of a proposed
  heating mechanism for the middle chromosphere is presented. The
  generalization consists of including the ideal gas equation of state,
  allowing the temperature to vary with position, and allowing the
  hydrogen flow velocity to vary with height in a specified manner. These
  generalizations allow for a self consistent calculation of a temperature
  profile. The variation of the flow velocity with height generates a
  component of the inertial force which adds to the vertical gradient
  of the thermal pressure in supporting the plasma against gravity. This
  allows for a lower temperature for a given number density. The solutions
  presented suggest that resistively heated magnetic loops embedded in
  a much stronger, larger scale potential field, and having horizontal
  spatial scales of several thousand kilometers provide the thermal energy
  necessary to heat the middle chromosphere on these spatial scales. For
  these solutions the temperature is in the range of 6000-8700K,
  consistent with the temperature range in the middle chromosphere. The
  magnetic loops have one footpoint region where the field is strongest
  and directed mainly upward, and where the heating rates per unit mass
  and volume are small. The field lines extend upward from this region at
  the base of the middle chromosphere, diverge horizontally, and return to
  a footpoint region at the base of the middle chromosphere as a weaker,
  more diffuse, mainly downward directed field. In this footpoint region
  the heating rates are also small. The heating rates are largest in the
  middle of the loops. For the magnetic loops considered, the temperature
  shows little horizontal variation between the footpoint region where
  the field is strongest and the heating rates are small, and the region
  where the heating rates are largest. This suggests that large horizontal
  variations in the net radiative loss from heated magnetic loops may not
  always be associated with large horizontal variations in temperature.

Title: Convection driven heating of the solar middle chromosphere
    by resistive dissipation of large scale electric currents.
Authors: Goodman, M. L.
Bibcode: 1997A&A...324..311G
Altcode:
  A two dimensional, steady state, resistive magnetohydrodynamic (MHD)
  model with flow is used to support the proposition that a major
  source of heating for the solar middle chromosphere is resistive
  dissipation of large scale electric currents driven by a convection
  electric field. The currents are large scale in that their scale
  heights range from hundreds of kilometers in the network to thousands
  of kilometers in the internetwork. The current is carried by protons,
  and flows orthogonal to the magnetic field in a weakly ionized, strongly
  magnetized hydrogen plasma. The flow velocity is mainly parallel to
  the magnetic field. The relatively small component of flow velocity
  orthogonal to the magnetic field generates a convection electric field
  which drives the current. The magnetic field is the sum of a loop
  shaped field, called a magnetic element, and a much stronger, larger
  scale potential field. All of the heating takes place in the magnetic
  element. Solutions to the model indicate that magnetic elements with
  horizontal spatial extents of about one thousand to five thousand
  kilometers may be confined to, and heat, the middle chromospheric
  network. Other solutions to the model indicate that magnetic elements
  with horizontal spatial extents of about ten thousand to thirty thousand
  kilometers may span and heat the middle chromospheric internetwork,
  and may be the building blocks of the chromospheric magnetic canopy. It
  is suggested that the middle chromosphere is highly structured over
  a wide range of spatial scales determined by the properties of these
  magnetic elements, and stronger, larger scale potential fields.

Title: MHD Modeling of the Transition Region Using Realistic Transport
    Coefficients
Authors: Goodman, Michael L.
Bibcode: 1997SPD....28.0604G
Altcode: 1997BAAS...29..910G
  Most of the transition region (TR) consists of a collision dominated
  plasma. The dissipation and transport of energy in such a plasma
  is accurately described by the well known classical transport
  coefficients which include the electrical and thermal conductivity,
  viscosity, and thermo- electric tensors. These tensors are anisotropic
  and are functions of local values of temperature, density, and
  magnetic field. They may be used in an MHD model to obtain a self
  consistent, physically realistic description of the TR. The physics of
  kinetic processes is included in the MHD model through the transport
  coefficients. As a first step in studying heating and cooling processes
  in the TR in a realistic, quantitative manner, a 1.5 dimensional, steady
  state MHD model with a specified temperature profile is considered. The
  momentum equation includes the inertial, pressure gradient, Lorentz,
  and gravitational forces. The Ohm's law includes the exact expressions
  for the electrical conductivity and thermo- electric tensors. The
  electrical conductivity relates the generalized electric field to the
  conduction current density while the thermo-electric tensor relates
  the temperature gradient to the thermo-electric current density. The
  total current density is the sum of the two. It is found that the
  thermo-electric current density can be as large as the conduction
  current density, indicating that thermo-electric effects are probably
  important in modeling the dynamics of energy dissipation, such as
  wave dissipation, in the TR. Although the temperature gradient is
  in the vertical direction, the thermo-electric current density is in
  the horizontal direction, indicating the importance of the effects of
  anisotropic transport. The transport coefficients are valid for all
  magnetic field strengths, and so may be used to study the physics of
  weakly as well as strongly magnetized regions of the TR. Numerical
  examples are presented.

Title: Heating of the Solar Middle Chromospheric Network and
    Internetwork by Large-Scale Electric Currents in Weakly Ionized
    Magnetic Elements
Authors: Goodman, Michael L.
Bibcode: 1996ApJ...463..784G
Altcode:
  A two-dimensional, dissipative magnetohydrodynamic model is used to
  argue that a major source of in situ heating for the solar middle
  chromosphere is the resistive dissipation of large-scale electric
  currents flowing in magnetic elements. A magnetic element is an
  arch-shaped magnetic field configuration consisting of a central
  region of horizontally localized, mainly vertical magnetic field
  based in the photosphere, with field lines that diverge horizontally
  with increasing height, extend into the middle chromosphere, and then
  return to the photo sphere as a relatively diffuse, weaker field. The
  currents that flow in these elements are carried by protons, and are
  large scale in that their scale height is hundreds of kilometers in
  the network and thousands of kilometers in the internetwork. Solutions
  to the model demonstrate that the resistive dissipation of large-scale
  electric currents flowing orthogonal to the magnetic field in magnetic
  elements embedded in a weakly ionized, strongly magnetized hydrogen
  gas may generate all of the thermal energy necessary to heat the middle
  chromosphere. The magnetic field is computed self-consistently with the
  electric field, pressure, and hydrogen and proton densities. Solutions
  to the model suggest that magnetic elements with horizontal extents up
  to several arcseconds may be confined to, and heat, the chromospheric
  network, while elements with the largest horizontal extents may span and
  heat the internetwork and be the building blocks of the chromospheric
  magnetic canopy. The model predicts that the heating rate per unit mass
  (q) is independent of height, peaked near but horizontally displaced
  from the center of a magnetic element, and for realistic model input
  parameters has an average value computed over the base area of the
  element dose to the value 4.5 x 10<SUP>9</SUP> ergs g<SUP>-1</SUP>
  s<SUP>-1</SUP> predicted by semiempirical models of the chromosphere
  that also predict that q is independent of height in the middle
  chromosphere. The model predicts that the heating rate per unit volume
  is peaked near the horizontal midpoint of a magnetic element where
  the field is mainly horizontal. The model predicts that both heating
  rates are zero at the center and outer boundary of a magnetic element
  where the field is vertical. These model predictions for the spatial
  localization of the heating rates are consistent with observations
  that regions of enhanced emission are near but horizontally displaced
  from regions of vertical, high-magnitude magnetic field.

Title: Convection Driven Heating of the Solar Middle Chromosphere
    by Large Scale Electric Currents
Authors: Goodman, M. L.
Bibcode: 1996AAS...188.3607G
Altcode: 1996BAAS...28..874G
  A two dimensional, steady state, resistive MHD model with flow is
  used to support the proposition that a major source of heating for the
  solar middle chromosphere is the resistive dissipation of large scale
  electric currents driven by a convection electric field. The currents
  are large scale in the sense that their scale heights range from
  hundreds of kilometers in the network to thousands of kilometers in the
  internetwork. The current is carried by protons, and flows orthogonal
  to the magnetic field which is embedded in a weakly ionized, strongly
  magnetized hydrogen plasma. The resistive dissipation is determined by
  the Pedersen resistivity. The flow velocity is mainly parallel to the
  magnetic field, but the relatively small component of flow velocity
  orthogonal to the magnetic field generates a convection electric field
  which drives the current. The magnetic field is the sum of a loop shaped
  field, and a much stronger, larger scale potential field. The heating
  takes place in the region occupied by the loop field which is only a few
  gauss while the potential field is close to 200 G. Hence magnetometer
  observations may suggest that the total field is potential while
  radiation intensity observations indicate the presence of mechanical
  heating. Solutions to the model indicate that magnetic elements with
  horizontal spatial extents of ~ 1 - 5 thousand kilometers may be
  confined to, and heat, the middle chromospheric network. Solutions to
  the model also indicate that magnetic elements with horizontal spatial
  extents of ~ 10 - 30 thousand kilometers may span and heat the middle
  chromospheric internetwork region over the interior of supergranules,
  and may be the building blocks of the chromospheric magnetic canopy.

Title: A three-dimensional, iterative mapping procedure for the
    implementation of an ionosphere-magnetosphere anisotropic Ohm's law
    boundary condition in global magnetohydrodynamic simulations
Authors: Goodman, Michael L.
Bibcode: 1995AnGeo..13..843G
Altcode: 1995AnG....13..843G
  The mathematical formulation of an iterative procedure for the numerical
  implementation of an ionosphere-magnetosphere (IM) anisotropic Ohm's
  law boundary condition is presented. The procedure may be used in
  global magnetohydrodynamic (MHD) simulations of the magnetosphere. The
  basic form of the boundary condition is well known, but a well-defined,
  simple, explicit method for implementing it in an MHD code has not been
  presented previously. The boundary condition relates the ionospheric
  electric field to the magnetic field-aligned current density driven
  through the ionosphere by the magnetospheric convection electric field,
  which is orthogonal to the magnetic field B, and maps down into the
  ionosphere along equipotential magnetic field lines. The source of
  this electric field is the flow of the solar wind orthogonal to B. The
  electric field and current density in the ionosphere are connected
  through an anisotropic conductivity tensor which involves the Hall,
  Pedersen, and parallel conductivities. Only the height-integrated
  Hall and Pedersen conductivities (conductances) appear in the final
  form of the boundary condition, and are assumed to be known functions
  of position on the spherical surface R=R1 representing the boundary
  between the ionosphere and magnetosphere. The implementation presented
  consists of an iterative mapping of the electrostatic potential
  &lt;psi&gt;, the gradient of which gives the electric field,
  and the field-aligned current density between the IM boundary at
  R=R1 and the inner boundary of an MHD code which is taken to be at
  R<SUB>2</SUB>&gt;R<SUB>1</SUB>. Given the field-aligned current density
  on R=R<SUB>2</SUB>, as computed by the MHD simulation, it is mapped
  down to R=R<SUB>1</SUB> where it is used to compute &lt;psi&gt; by
  solving the equation that is the IM Ohm's law boundary condition. Then
  &lt;psi&gt; is mapped out to R=R<SUB>2</SUB>, where it is used to
  update the electric field and the component of velocity perpendicular
  to &lt;strong&gt;B&lt;/strong&gt;. The updated electric field and
  perpendicular velocity serve as new boundary conditions for the MHD
  simulation which is then used to compute a new field-aligned current
  density. This process is iterated at each time step. The required Hall
  and Pedersen conductances may be determined by any method of choice,
  and may be specified anew at each time step. In this sense the coupling
  between the ionosphere and magnetosphere may be taken into account in
  a self-consistent manner.

Title: Heating of the Solar Middle Chromosphere by Large-Scale
    Electric Currents
Authors: Goodman, M. L.
Bibcode: 1995ApJ...443..450G
Altcode:
  A global resistive, two-dimensional, time-dependent magnetohydrodynamic
  (MHD) model is used to introduce and support the hypothesis that the
  quiet solar middle chromosphere is heated by resistive dissipation
  of large-scale electric currents which fill most of its volume. The
  scale height and maximum magnitude of the current density are 400 km
  and 31.3 m/sq m, respectively. The associated magnetic field is almost
  horizontal, has the same scale height as the current density, and has
  a maximum magnitude of 153 G. The current is carried by electrons
  flowing across magnetic field lines at 1 m/s. The resistivity is
  the electron contribution to the Pedersen resitivity for a weakly
  ionized, strongly magnetized, hydrogen gas. The model does not include
  a driving mechanism. Most of the physical quantities in the model
  decrease exponentially with time on a resistive timescale of 41.3
  minutes. However, the initial values and spatial; dependence of these
  quantities are expected to be essentially the same as they would be if
  the correct driving mechanism were included in a more general model. The
  heating rate per unit mass is found to be 4.5 x 10<SUP>9</SUP>
  ergs/g/s, independent of height and latitude. The electron density
  scale height is found to be 800 km. The model predicts that 90% of the
  thermal energy required to heat the middle chromosphere is deposited
  in the height range 300-760 km above the temperature minimum. It is
  shown to be consistent to assume that the radiation rate per unit
  volume is proportional to the magnetic energy density, and then it
  follows that the heating rate per unit volume is also proportional to
  the energy from the photosphere into the overlying chromosphere are
  briefly discussed as possible driving mechanisms for establishing and
  maintaining the current system. The case in which part of or all of the
  current is carried by protons and metal ions, and the contribution of
  electron-proton scattering to the current are also considered, with the
  conclusion that these effects do not change the qualitative prediction
  of the model, but probably change the quantitative predictions slightly,
  mainly by increasing the maximum magntiude of the current density and
  magnetic field to at most approximately 100 mA/m and approximately 484
  G, respectively. The heating rate per unit mass, current density scale
  height, magnetic field scale height, temperatures, and pressures are
  unchanged or are only slightly changed by including these additional
  effects due to protons and ions.

Title: Neutrino Oscillation Experiments with Atmospheric Neutrinos
Authors: Gaisser, T.; Goodman, M.
Bibcode: 1995pnac.conf..220G
Altcode:
  No abstract at ADS

Title: Long-Baseline Neutrino Oscillation Experiments
Authors: Crane, D.; Goodman, M.
Bibcode: 1995pnac.conf..225C
Altcode:
  No abstract at ADS

Title: Long-baseline neutrino oscillation experiments
Authors: Crane, D.; Goodman, M.
Bibcode: 1994panm.conf.....C
Altcode:
  There is no unambiguous definition for long baseline neutrino
  oscillation experiments. The term is generally used for accelerator
  neutrino oscillation experiments which are sensitive to Delta sq m
  less than 1.0 eV<SUP>2</SUP>, and for which the detector is not on the
  accelerator site. The Snowmass N2L working group met to discuss the
  issues facing such experiments. The Fermilab Program Advisory Committee
  adopted several recommendations concerning the Fermilab neutrino program
  at their Aspen meeting immediately prior to the Snowmass Workshop. This
  heightened the attention for the proposals to use Fermilab for a
  long-baseline neutrino experiment at the workshop. The plan for
  a neutrino oscillation program at Brookhaven was also thoroughly
  discussed. Opportunities at CERN were considered, particularly the
  use of detectors at the Gran Sasso laboratory. The idea to build a
  neutrino beam from KEK towards Superkamiokande was not discussed at
  the Snowmass meeting, but there has been considerable development of
  this idea since then. Brookhaven and KEK would use low energy neutrino
  beams, while FNAL and CERN would plan have medium energy beams. This
  report will summarize a few topics common to LBL proposals and attempt
  to give a snapshot of where things stand in this fast developing field.

Title: Driven, dissipative, energy-conserving magnetohydrodynamic
    equilibria. Part 2. The screw pinch
Authors: Goodman, Michael L.
Bibcode: 1993JPlPh..49..125G
Altcode:
  A cylindrically symmetric, electrically driven, dissipative,
  energy-conserving magnetohydrodynamic equilibrium model is
  considered. The high-magneticfield Braginskii ion thermal conductivity
  perpendicular to the local magnetic field and the complete electron
  resistivity tensor are included in an energy equation and in
  Ohm's law. The expressions for the resistivity tensor and thermal
  conductivity depend on number density, temperature, and the poloidal
  and axial (z-component) magnetic field, which are functions of radius
  that are obtained as part of the equilibrium solution. The model has
  plasma-confining solutions, by which is meant solutions characterized
  by the separation of the plasma into two concentric regions separated
  by a transition region that is an internal boundary layer. The inner
  region is the region of confined plasma, and the outer region is
  the region of unconfined plasma. The inner region has average values
  of temperature, pressure, and axial and poloidal current densities
  that are orders of magnitude larger than in the outer region. The
  temperature, axial current density and pressure gradient vary rapidly
  by orders of magnitude in the transition region. The number density,
  thermal conductivity and Dreicer electric field have a global minimum
  in the transition region, while the Hall resistivity, Alfvén speed,
  normalized charge separation, Debye length, (ωλ)<SUB>ion</SUB>
  and the radial electric field have global maxima in the transition
  region. As a result of the Hall and electron-pressure-gradient
  effects, the transition region is an electric dipole layer in which
  the normalized charge separation is localized and in which the radial
  electric field can be large. The model has an intrinsic value of β,
  about 13·3%, which must be exceeded in order that a plasma-confining
  solution exist. The model has an intrinsic length scale that, for
  plasma-confining solutions, is a measure of the thickness of the
  boundary-layer transition region. If appropriate boundary conditions
  are given at R = 0 then the equilibrium is uniquely determined. If
  appropriate boundary conditions are given at any outer boundary R
  = a then the equilibrium exhibits a bifurcation into two states,
  one of which exhibits plasma confinement and carries a larger axial
  current than the other, which is almost homogeneous and cannot confine
  a plasma. Exact expressions for the two values of the axial current in
  the bifurcation are derived. If the boundary conditions are given at R =
  a then a solution exists if and only if the constant driving electric
  field exceeds a critical value. An exact expression for this critical
  electric field is derived. It is conjectured that the bifurcation is
  associated with an electric-field-driven transition in a real plasma,
  between states with different rotation rates, energy dissipation rates
  and confinement properties. Such a transition may serve as a relatively
  simple example of the L—H mode transition observed in tokamaks.

Title: On driven, dissipative, energy-conserving magnetohydrodynamic
    equilibria
Authors: Goodman, Michael L.
Bibcode: 1992JPlPh..48..177G
Altcode:
  A cylindrically symmetric, electrically driven, dissipative,
  energy-conserving magnetohydrodynamic equilibrium model is
  considered. The high-magnetic-field Braginskii electron electrical
  resistivity η parallel to a constant axial magnetic field B and
  ion thermal conductivity ĸ perpendicular to B are included in an
  energy equation and in Ohm's law. The expressions for η and ĸ
  depend on number density and temperature, which are functions of
  radius that are obtained as part of the equilibrium solution. The
  model has plasma-confining solutions, by which are meant solutions
  characterized by the separation of the plasma into two regions separated
  by a relatively thin transition region that is an internal boundary
  layer across which temperature and current density vary rapidly. The
  inner region has a temperature, pressure and current density that are
  much larger than in the outer region. The number density and thermal
  conductivity attain their minimum values in the transition region. The
  model has an intrinsic value of β, about 6.6%, which must be exceeded
  in order that a plasma-confining solution exist. The model has an
  intrinsic length scale, which, for plasma-confining solutions, is a
  measure of the thickness of the transition region separating the inner
  and outer regions of plasma. A larger class of transport coefficients
  is modelled by artificially changing η and ĸ by changing the constant
  coefficients η<SUB>O</SUB> and ĸ<SUB>O</SUB> that occur in their
  expressions. Increasing ĸ<SUB>O</SUB> transforms a state that does
  not exhibit confinement into one that does, improves the confinement
  in a state that already exhibits it, and leads to an increase in ĸ in
  the confined region of plasma. The improvement in confinement consists
  in a decrease in the thickness of the transition region. Decreasing
  η<SUB>O</SUB> subject to certain constraints, also transforms a state
  that does not exhibit confinement into one that does, improves the
  confinement in a state that already exhibits it, and leads to a decrease
  in η in the confined region of plasma. Increasing η<SUB>O</SUB> up to
  a critical point increases the current, temperature, and volume of the
  confined region of plasma, and causes the thickness of the transition
  region to increase. If η<SUB>O</SUB> is increased beyond the critical
  point, a plasma-confining state cannot exist. In all cases it is found
  that an increase in ĸ and a decrease in η in the confined region of
  plasma are associated with an improvement in the confinement properties
  of the equilibrium state. If the pressure and temperature are given on
  the cylinder wall, the equilibrium bifurcates when the electric field
  decreases below a critical value. The equilibrium can bifurcate into
  a state that exhibits confinement and a state that does not.

Title: Coincidences between extensive air showers and the Soudan 1
    underground muon detector
Authors: Das Gupta, U.; Border, P.; Johns, K.; Longley, N.; Marshak,
   M.; Peterson, E.; Ruddick, K.; Shupe, M.; Ayres, D.; Dawson, J.;
   Fields, T.; Goodman, M.; May, E.
Bibcode: 1992PhRvD..45.1459D
Altcode:
  We have operated the Soudan 1 underground muon detector in coincidence
  with a 36-m<SUP>2</SUP> detector situated at the Earth's surface. Such
  a combination of detectors can yield information on the composition
  of the primary cosmic rays at energies above ~3×10<SUP>15</SUP>
  eV, where there is an abrupt change in the slope of the energy
  spectrum. The present experiment was meant to test the feasibility of
  operating such a system, and to obtain a first sample of data before
  the complete installation of the much larger Soudan 2 detector. These
  initial data seem to favor a light composition in the energy range
  10<SUP>15</SUP>-10<SUP>16</SUP> eV, but there are significant systematic
  uncertainties.

Title: Combination of Probabilities in Looking for Cosmic Ray Sources
Authors: Goodman, M.
Bibcode: 1991ICRC....2..660G
Altcode: 1991ICRC...22b.660G
  No abstract at ADS

Title: Signals from cosmic ray sources, some statistical issues
Authors: Goodman, M.
Bibcode: 1990hep..conf.....G
Altcode:
  The possible existence of discrete sources of cosmic rays is presently
  one of the main topics of study in non-accelerator particle physics. The
  search is being conducted in a wide variety of experiments using
  UHE gamma rays, VHE gamma rays, EeV particles, underground mu's and
  nu's. The current experimental situation, however, can be described as
  chaotic. The number of claimed observations of sources by different
  groups using a variety of experimental techniques is quite large,
  but a consistent interpretation of the various results has failed
  to emerge. Most of the observations rely on either a dc excess from
  the direction of the source, a periodicity of the events from that
  direction, or some combination of these two effects. In the first
  section of this paper, we discuss some of the techniques that may be
  used in searching for a dc excess. We review two common bin free tests
  of the light curves. We discuss a particular problem involving phase
  coherence when doing a period search. This paper discusses some of
  the issues and meanings involved in combining probabilities from more
  than one test. Prescribing the right way to do analysis is certainly
  beyond this paper's scope. However some of the issues and problems
  are considered here.

Title: Cosmic ray air showers in a fine grained calorimeter.
Authors: Goodman, M.
Bibcode: 1986isos.book..568G
Altcode:
  No abstract at ADS

Title: An Experimental Study of Hadrons and Muons Near Shower Cores
    Using the E-594 Neutrino Detector at Fermilab
Authors: Goodman, J. A.; Tonwar, S. C.; Yodh, G. B.; Ellsworth,
   R. W.; Goodman, M.; Bogert, D.; Brock, R.; Burnstein, R.; Fuess, S.;
   Morfin, J.; Peters, M.; Stutte, L.; Walter, J. K.; Bofill, J.; Busza,
   W.; Friedman, J.; Lyons, T.; Mattison, T.; Osborne, L. B.; Pitt, R.;
   Rosenson, L.; Sandacz, A.; Tartaglia, M.; Whitaker, S.; Yeh, G. P.;
   Abolins, M.; Cohen, A.; Owen, D.; Slate, J.; Taylor, F. E.; Mukherjee,
   A.; Eldridge, T.; Magahiz, R.
Bibcode: 1983ICRC...11..248G
Altcode: 1983ICRC...18k.248G; 1983icrc...11..248G
  The E-594 neutrino detector has been used to study the lateral
  distribution of hadrons and muons near shower cores. The detector
  consists of a 340-ton fine-grain calorimeter with 400,000 cells of
  flash chamber and dimensions 3.7 x 20 x 3.7 m (height). The average
  density of absorber in the calorimeter is 1.4 g/sq cm and the average
  Z is 21. A 5-day run was taken on cosmic-ray data using a trigger
  provided by four 0.6-sq m plastic scintillation counters located above
  the calorimeter. A shower density of eight particles/sq m was required
  to trigger. These data were studied to determine the number of muons
  traversing the device as a function of electron density. Preliminary
  results of this study are compared to Monte Carlo simulations of air
  showers from hadrons of 1-10 PeV.

Title: An Experimental Study of Hadrons and Muons Near Shower Cores
    Using the E-594 Neutrino Detector at Fermilab
Authors: Yodh, G. B.; Goodman, J. A.; Tonwar, S. C.; Ellsworth, R. W.;
   Goodman, M.
Bibcode: 1983ICRC....6...70Y
Altcode: 1983ICRC...18f..70Y
  No abstract at ADS