Diagnostics of flarе plasma from X-ray and EUV observations: mechanisms of energy release and radiation

  • Yu.T. Tsap Crimean Astrophysical Observatory
  • G.G. Motorina Главная (Пулковская) астрономическая обсерватория РАН, Пулковское шоссе, 65/1, Санкт-Петербург, Россия, 196140
  • Yu.G. Kopylova Главная (Пулковская) астрономическая обсерватория РАН, Пулковское шоссе, 65/1, Санкт-Петербург, Россия, 196140

Abstract

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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Published
2016-11-10
How to Cite
Tsap Y., Motorina G., Kopylova Y., 2016. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 112, no. 2, pp. 137-145. Available at: https://jn.craocrimea.ru/index.php/izvcrao/article/view/194 (Accessed: 2December2020)
Section
Сonference proceedings