SH012
Fundamental Physics of the Solar Corona and Inner Heliosphere
Fundamental Physics of the Solar Corona and Inner Heliosphere
Session ID#: 157259
Session Description:
The inner heliosphere provides a natural laboratory to understand how magnetized plasmas are heated, accelerated and structured over a wide range of time and spatial scales. This session explores the many facets of physical processes involved in the origins of the turbulent, super-Alfvénic wind filling the heliosphere: How do magnetic structure and local processes at the sources in the solar atmosphere determine different wind types? How do distribution functions evolve, from the thermal population to energetic particle acceleration? What are the roles of turbulence and wave-particle interactions in heating and acceleration of the solar corona and wind? How is the energization associated with structures, such as switchbacks, shocks, compression regions, current sheets and magnetic reconnection?
Now in its eighth year, this session welcomes theoretical, numerical simulation, and observational papers, including contributions stemming from Parker Solar Probe, Solar Orbiter, BepiColombo and the whole Heliophysics System Observatory, as well as developments and new challenges inspired by such observations.
Index Terms:
2159 Plasma waves and turbulence [INTERPLANETARY PHYSICS]
2164 Solar wind plasma [INTERPLANETARY PHYSICS]
2169 Solar wind sources [INTERPLANETARY PHYSICS]
7509 Corona [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
Primary Convener: Marco C M Velli, University of California Los Angeles, Los Angeles, CA, United States
Conveners: Chadi S Salem, University of California, Berkeley, CA, United States, Olga Panasenco, Advanced Heliophysics Inc., Pasadena, United States and Yannis Zouganelis, European Space Agency, Villanueva De La Can, Spain
Student/Early Career Convener: Chen Shi, University of California, Los Angeles, Los Angeles, United States
See more of: SPA-Solar and Heliospheric Physics
