Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2701r&link_type=abstract
American Astronomical Society, SPD meeting #37, #27.01; Bulletin of the American Astronomical Society, Vol. 38, p.253
Astronomy and Astrophysics
Astrophysics
Scientific paper
This dissertation develops a theoretical model for the radiative output of eruptive solar flares. The new model is based on an earlier one by Lin & Forbes (2000), in which a flux rope in equilibrium in the corona is made to erupt due to a catastrophic loss of equilibrium. After the eruption, a vertical current sheet forms underneath the flux rope. Here, we calculate the thermal energy released by this process under the assumption that all of the Poynting flux into the current sheet is thermalized. We use the calculated thermal energy release from the model to determine thermal flare emissions at various wavelengths as a function of time. We find that cases with large background fields (which produce fast CMEs) produce large amounts of flare emission, while cases with weak background magnetic fields (which produce slow CMEs) produce weak flare emission. In addition, we find that observations of bright, loop-top "knots'' of flare emission can be explained by a flare arcade with multiple loops sequentially undergoing heating and chromospheric evaporation. We also find that a sensitive enough instrument should be able to detect blueshifts in flare spectra due to chromospheric evaporation early in the flare evolution. This work was supported the National Science Foundation and the New Hampshire Space Grant Consortium.
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