HR: 1330h
AN: SH22A-0175    [PDF]
TI: Radiative Hydrodynamic Models of Solar White Light Flares
AU: * Allred, J C
EM: allred@astro.washington.edu
AF: University of Washington, Department of Astronomy, Box 351580, Seattle, WA 98195 United States
AU: Hawley, S L
EM: slh@astro.washington.edu
AF: University of Washington, Department of Astronomy, Box 351580, Seattle, WA 98195 United States
AU: Abbett, W P
EM: abbett@ssl.berkeley.edu
AF: UC Berkeley, Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Fisher, G H
EM: fisher@ssl.berkeley.edu
AF: UC Berkeley, Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Hudson, H S
EM: hhudson@ssl.berkeley.edu
AF: UC Berkeley, Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Metcalf, T R
EM: metcalf@lmsal.com
AF: Lockheed Martin ATC, Solar & Astrophysics Laboratory, Dept. L9-41, Palo Alto, CA 94304 United States
AB: We report on theoretical radiative hydrodynamic simulations of solar white light flares. The solar atmosphere is modeled in detail from the transition region to the photosphere. The coronal pressure and X-ray backheating are included self-consistently. Flare heating is assumed to be from an electron beam which is modeled for several white light flares using data from RHESSI, TRACE and Yohkoh. We also investigate the possibility that the 511 keV line width is produced from a significant column depth of atmosphere at transition region temperatures. We compare our new solar flare models to previous results, and to models of M dwarf stellar flares.
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7539 Stellar astronomy
DE: 7546 Transition region
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting