SH42A:
Fundamental Physics of the Solar Corona and Inner Heliosphere I

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Session ID#: 15861

Session Description:
The solar corona and solar wind provide a complex laboratory where magnetic fields guide and energize the plasma. Structured over an incredibly wide range of time and spatial scales, the coronal plasma is heated and accelerated to give the turbulent, super-Alfvénic wind observed in the heliosphere. This session is open to exploring the many facets of physical processes involved in heliospheric origins: from the sources of different wind types and their connection to coronal structures, to the micro-physics of distribution functions, anisotropies, to the role of turbulence and wave-particle interactions in heating and acceleration, to the energization associated with structures, such as shocks, current sheets and magnetic reconnection. What specific observables can be derived from models, what fundamental observations should drive theoretical developments, in preparation for the decade of inner heliospheric and coronal exploration with Solar Orbiter and Solar Probe Plus? Solicited contributions include theoretical, numerical simulation, and observational papers.
Primary Convener:  Chadi S Salem, SSL, University of California Berkeley, Berkeley, United States
Conveners:  Marco C M Velli, University of California Los Angeles, Los Angeles, CA, United States and Olga Panasenco, Advanced Heliophysics Inc., Pasadena, CA, United States
Chairs:  Marco C M Velli, University of California Los Angeles, Los Angeles, CA, United States, Olga Panasenco, Advanced Heliophysics Inc., Pasadena, CA, United States and Chadi S Salem, SSL, University of California Berkeley, Berkeley, United States
OSPA Liaison:  Olga Panasenco, Advanced Heliophysics Inc., Pasadena, CA, United States
Index Terms:

2164 Solar wind plasma [INTERPLANETARY PHYSICS]
2169 Solar wind sources [INTERPLANETARY PHYSICS]
7509 Corona [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
7524 Magnetic fields [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]

Abstracts Submitted to this Session:

Fundamental Physics of the Slow Solar Wind - What do we Know? (Invited) (123473)
Leon Ofman, NASA GSFC/CUA, Greenbelt, United States, Lucia Abbo, Astrophysical Observatory of Turin, Pino Torinese, Italy, Spiro K Antiochos, NASA Goddard Space Flight Center, Greenbelt, United States, Viggo Haraldson Hansteen, Institute for Theoretical Astrophysics, University of Oslo, Oslo, Norway, Louise Harra, University College London, London, United Kingdom, Yuan-Kuen Ko, US Naval Research Laboratory, Space Science Division, Washington, DC, United States, Giovanni Lapenta, KU Leuven, Mathematics, Leuven, Belgium, Bo Li, Shandong University at Weihai, Weihai, China, Pete Riley, Predictive Science Inc., San Diego, CA, United States, Leonard Strachan, US Naval Research Laboratory, Washington, DC, United States, Rudolf von Steiger, International Space Science Institute, Bern, Switzerland and Yi-Ming Wang, US Naval Research Laboratory, Washington, United States
Alfvénic Slow Solar Wind: characteristics and origin (Invited) (124005)
Raffaella D'Amicis, IAPS-INAF, Rome, Italy
Collisionless Isotropization of the Solar-Wind Protons by Compressive Fluctuations and Plasma Instabilities (126701)
Daniel Verscharen, University of New Hampshire, Space Science Center, Durham, United States, Benjamin D G Chandran, University of New Hampshire, Durham, United States, Prof. Kristopher Gregory Klein, University of New Hampshire, Durham, NH, United States; University of Michigan Ann Arbor, Ann Arbor, MI, United States and Eliot Quataert, Princeton University, Princeton, NJ, United States
Constraining heating processes in the solar wind with kinetic properties of heavy ions (138254)
Patrick Tracy1, Thomas Zurbuchen1, Justin Christophe Kasper2, Jim M Raines2, Jason A Gilbert2 and Paul Shearer1, (1)University of Michigan Ann Arbor, Ann Arbor, MI, United States, (2)University of Michigan Ann Arbor, Climate and Space Sciences and Engineering, Ann Arbor, MI, United States
Heating of protons and electrons in plasma turbulence: theory and simulation (152648)
Prof. William H Matthaeus1, Tulasi Parashar1, Minping Wan2 and Pin Wu3, (1)University of Delaware, Department of Physics and Astronomy, Newark, DE, United States, (2)South University of Science and Technology of China, Shenzhen, Guangdong 518055, China, (3)University of Delaware, Newark, DE, United States
OBSERVATIONAL SIGNATURES OF CORONAL HEATING (173939)
Russell B. Dahlburg1, Giorgio Einaudi2, Ignacio Ugarte-Urra1, Harry P Warren3, Antonio F Rappazzo4, Marco C M Velli5 and Brian Taylor6, (1)US Naval Research Laboratory, Washington, DC, United States, (2)Berkeley Research Associates, Inc., Berkeley, CA, United States, (3)Naval Research Laboratory, Washington, DC, United States, (4)UCLA, Earth, Planetary and Space Sciences, Pasadena, CA, United States, (5)University of California Los Angeles, Los Angeles, CA, United States, (6)AIr Force Research Laboratory Eglin - afrl, Valparaiso, FL, United States
Runaway Signatures in the Transport Description of Solar Wind Electrons: A New Quantitative Steady Electron Runaway Model (SERM) (134767)
Jack D Scudder, University of Iowa, Iowa City, IA, United States and Chadi S Salem, SSL, University of California Berkeley, Berkeley, United States
Regulation of pressure anisotropy in the solar wind: processes within inertial range of turbulence (183135)
Marek Strumik1, Alexander A Schekochihin1, Jonathan Squire2 and Stuart D Bale3, (1)University of Oxford, Oxford, United Kingdom, (2)California Institute of Technology, Pasadena, CA, United States, (3)University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, United States

See more of: SPA-Solar and Heliospheric Physics