Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2209c&link_type=abstract
American Astronomical Society, SPD meeting #42, #22.09; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) has shown that super-hot (T > 30 MK) thermal plasmas occur frequently in intense, GOES X-class solar flares. Recent analysis suggests that such hot plasmas are substantially heated directly within the corona, and are both spatially and physically distinct from the usual 10-20 MK "GOES-temperature" plasma formed by chromospheric evaporation. During the 2002 July 23 X4.8 flare, a strong non-thermal source is observed in the corona prior to the impulsive phase, and is taken to signal the onsent of particle acceleration by magnetic reconnection. A cospatial thermal source is also observed, but its temperature is only loosely constrained. During the impulsive phase proper, a 60-100 keV HXR source is briefly observable in the corona; new imaging analysis shows that it is cospatial with a 36 MK super-hot source, whose temperature at this time is well-determined and which lies above the SXR-emitting GOES-temperature loops. A preliminary analysis indicates that this HXR source is distinctly non-thermal, and its timing suggests a second episode of magnetic reconnection further along the flaring arcade; the super-hot source may be located directly within the acceleration region, or at least presents a suitably-dense target for the emission of 60-100 keV hard X-rays. We discuss these observations, and their implications for particle acceleration and plasma heating in X-class flares.
Caspi Amir
Lin Robert P.
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