Using a Loss-of-Equilibrium CME Model to Predict X-Ray and EUV Emissions Resulting From Solar Flares

Details Using a Loss-of-Equilibrium CME Model to Predict X-Ray and EUV Emissions Resulting From Solar Flares Using a Loss-of-Equilibrium CME Model to Predict X-Ray and EUV Emissions Resulting From Solar Flares

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..68r&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

Physics

Scientific paper

In this study, we use a loss-of-equilibrium model for solar eruptions to calculate the thermal energy input into a system of flare loops. In this model, the flare consists of a system of reconnecting loops below a current sheet that connects the flare to an erupting flux rope. The thermal energy is calculated by assuming that all of the Poynting flux into the current sheet is thermalized. The density, temperature and velocity of the plasma in each reconnected loop are then calculated using a 1D hydrodynamic code. These parameters are coupled with the instrument response functions of various solar instruments to calculate flare emissions. We simulate spectra from the Bragg Crystal Spectrometer (BCS) on Yohkoh, and find that the strong blueshifts that should be present due to chromospheric evaporation during flare initiation are difficult to observe with BCS, but may be better observed with a more sensitive instrument. We also find that a density enhancement occurs at the top of a loop when evaporating plasma fronts in each loop leg collide there. This enhancement gives rise to bright loop-top intensities in simulated Transition Region and Coronal Explorer (TRACE) and Yohkoh Soft X-ray Telescope (SXT) images. These loop-top features have been observed in TRACE and SXT images, and are not explained by single-loop flare models. The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory should be able to observe these features in detail, and we will use this model to help develop flare observing programs for AIA.

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