Radiative Hydrodynamic Models of Solar White Light Flares

Details Radiative Hydrodynamic Models of Solar White Light Flares Radiative Hydrodynamic Models of Solar White Light Flares

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh22a0175a&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH22A-0175

Astronomy and Astrophysics

Astronomy

7514 Energetic Particles (2114), 7519 Flares, 7539 Stellar Astronomy, 7546 Transition Region

Scientific paper

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.

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