Solar flares: observations vs simulations

Details Solar flares: observations vs simulations Solar flares: observations vs simulations

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..274..182r&link_type=abstract

Advances in Plasma Astrophysics, Proceedings of the International Astronomical Union, IAU Symposium, Volume 274, p. 182-184

Astronomy and Astrophysics

Astrophysics

Methods: Numerical, Radiative Transfer, Sun: Atmosphere, Sun: Flares

Scientific paper

In order to study the properties of faint, moderate and bright flares, we simulate the conditions of the solar atmosphere using a radiative hydrodynamic model (Abbett & Hawley, 1999). A constant beam of non-thermal electrons is injected at the apex of a 1D coronal loop and heating from thermal soft X-ray emission is included. We compare the results with some observational data in Ly-α (using TRACE 1216 and 1600 Å data and estimating the ``pure'' Ly-α emission) and in Hα (data taken with a Multichannel Flare Spectrograph, at the Ondrejov Observatory).

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