Fundamental Physics of the Solar Corona and Inner Heliosphere
Fundamental Physics of the Solar Corona and Inner Heliosphere
Session ID#: 118540
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 does magnetic structure in the corona 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 compression regions, shocks, current sheets and magnetic reconnection? Now in its seventh year, this session welcomes theoretical, numerical simulation, and observational papers, including contributions stemming from Parker Solar Probe, Solar Orbiter, Bepi Colombo, as well as developments and new challenges inspired by such observations.
Co-Sponsor(s):
- EGU: European Geosciences Union -
Index Terms:
4490 Turbulence [NONLINEAR GEOPHYSICS]
7524 Magnetic fields [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
7835 Magnetic reconnection [SPACE PLASMA PHYSICS]
7846 Plasma energization [SPACE PLASMA PHYSICS]
Primary Convener: Marco C M Velli, University of California Los Angeles, Los Angeles, CA, United States
Conveners: Olga Panasenco, Advanced Heliophysics, Pasadena, CA, United States and Chadi S Salem, University of California, Berkeley, CA, United States
Primary Liaison: Yannis Zouganelis, European Space Agency, ESAC, Villanueva De La Can, Spain
See more of: SPA-Solar and Heliospheric Physics