Observations of the December 6, 2006 solar flare: Electron acceleration and plasma heating

Details Observations of the December 6, 2006 solar flare: Electron acceleration and plasma heating Observations of the December 6, 2006 solar flare: Electron acceleration and plasma heating

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010astl...36..430s&link_type=abstract

Astronomy Letters, Volume 36, Issue 6, pp.430-437

Astronomy and Astrophysics

Astronomy

Solar Flares, Solar Electromagnetic Radiation

Scientific paper

The flare plasma temperature calculated from GOES-11 (1.5-12.4 and 3.1-24.8 keV) data is compared with the solar nonthermal fluxes in various energy ranges in the December 6, 2006 event. Particle acceleration and plasma heating episodes took place in the pre-flare and impulsive phases; a hard ( ACS SPI > 150 keV) X-ray emission was observed 5 min before the onset of the GOES X-ray flare and was not accompanied by a temperature rise. A close correlation has been found between the flare plasma temperature and the hard X-ray intensity. The temperature delayed by 0.4 min turned out to be directly proportional to the logarithm of the ACS SPI count rate within the first 3 min of the impulsive phase. This shows that the accelerated electrons responsible for the X-ray emission were the main plasma heating source in the pre-flare and impulsive phases. The correlation between the temperature and the hard X-ray intensity disappears after the observation of a resonance peak at a frequency of 245 MHz. Significant electron fluxes may no longer be able to effectively heat the expanding plasma when its density in the interaction region reaches ˜109 cm-3. The observations of the July 23, 2002 and December 5, 2006 events confirm the trends found.

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