SH43C:
Multiwavelength Observations and Modeling of Solar Flares: Magnetic Structures, Particle Acceleration, and Atmospheric Response

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Session ID#: 31312

Session Description:
Solar flares are highly dynamic processes that can release significant amounts of thermal and non-thermal energy. How the energy is transported along the solar atmosphere and deposited in different layers as well as the relation between wave-heating, thermal, and non-thermal processes is still largely unknown. Similarly, the role of magnetic field topological structures and dynamic processes in the energy budget and energy release processes of a flare remain topics of discussion. High quality multi-wavelength and spectroscopic information with unprecedented spatial and temporal resolution from space and ground-based telescopes (e.g., RHESSI, MinXSS, IRIS, SDO, Hinode, NuSTAR, NoRH, and OVSA) together with advanced simulations can constrain the energy input and dissipation during a flare. The emission at each wavelength is associated with physical processes in different atmospheric layers. Studying the atmospheric response, thermal and non-thermal emissions, and magnetic field evolution are keys to understand the flare heating mechanism and energetic particle production.
Primary Convener:  Frederic Effenberger, Bay Area Environmental Research Institute, NASA Research Park, Moffet Field, CA, United States; International Space Science Institute, Bern, Switzerland
Conveners:  Fatima Rubio da Costa, Stanford University, Department of Physics, Stanford, CA, United States, Xudong Sun, Stanford University, Stanford, CA, United States and Lucia Kleint, University of Applied Sciences and Arts Northwestern Switzerland, Windisch, Switzerland
Chairs:  Frederic Effenberger, International Space Science Institute, Bern, Switzerland and Xudong Sun, Stanford University, Stanford, CA, United States
OSPA Liaison:  Fatima Rubio da Costa, Stanford University, Department of Physics, Stanford, CA, United States
Index Terms:

7514 Energetic particles [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
7519 Flares [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
7524 Magnetic fields [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]
7554 X-rays, gamma rays, and neutrinos [SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY]

Abstracts Submitted to this Session:

Comparing the Chromospheric Response to Different Flare Energy Transport Mechanisms (Invited) (228877)
Dr. Graham Stewart Kerr, PhD1, Jeffrey W Reep2, Joel C Allred3, Alexander J B Russell4, James Edward Leake1 and Lucas Tarr5, (1)NASA Goddard Space Flight Center, Greenbelt, United States, (2)Naval Research Lab DC, Washington, DC, United States, (3)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (4)University of Dundee, Dundee, DD1, United Kingdom, (5)Naval Research Laboratory, Washington, United States
Diffusive transport of energetic electrons in the solar corona: X-ray and radio diagnostics (253839)
Sophie Musset, ESTEC, Noordwijk, Netherlands, Eduard Kontar, University of Glasgow, Glasgow, G12, United Kingdom and Nicole Vilmer, Observatoire Paris, Meudon, France
High Resolution Flare Observations with the 1.6 m Telescope at Big Bear Solar Observatory (216632)
Haimin Wang, New Jersey Institute of Technology, Center for Solar-Terrestrial Research, Newark, United States
Tracing Fast Electron Beams Emanating from the Magnetic Reconnection Site in a Solar Jet (287289)
Bin Chen1, Sijie Yu1, Marina Battaglia2 and Sam Krucker3,4, (1)New Jersey Institute of Technology, Center for Solar-Terrestrial Research, Edison, NJ, United States, (2)University of Applied Sciences and Arts Northwestern Switzerland, Windisch, Switzerland, (3)FHNW, Windisch, Switzerland, (4)University of Applied Sciences Northwestern Switzerland and University of California Berkeley, Berkeley, United States
Numerical Modeling of Flare-productive Active Regions of the Sun (217298)
Shin Toriumi, NAOJ National Astronomical Observatory of Japan, Tokyo, Japan and Shinsuke Takasao, Nagoya University, Nagoya, Japan

See more of: SPA-Solar and Heliospheric Physics