Diagnostics of flarе plasma from X-ray and EUV observations: mechanisms of energy release and radiation
The estimates of the emission measure and temperature of coronal flare plasma derived from GOES, RHESSI, and SDO/AIA observations are compared. We found that the magnitude of plasma parameters can vary significantly (up to an order of magnitude) depending on the instrument, namely, a method of measurements and data processing. The advantages and disadvantages of these approaches are discussed. As a case study the November 9, 2013 flare was chosen. We found that electrons accelerated at a flaring loop’s top cannot maintain the observed hard X-ray fluxes at the loop footpoints. This might indicate that charged particles are additionally accelerated in the chromosphere.
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