Nonthermal X-ray Microflares

Details Nonthermal X-ray Microflares Nonthermal X-ray Microflares

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh24a..03c&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH24A-03

Other

7509 Corona, 7514 Energetic Particles (2114), 7519 Flares, 7537 Solar And Stellar Variability, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) provides unique sensitivity in the 3-15 keV energy range, with an effective area ˜100 times larger than similar past instruments. Along with its high spectral resolution (1 keV) RHESSI is uniquely suited to study small events. Microflares have been observed by Benz & Grigis (2002) and Krucker et al. (2002) to have anomalously steep spectra ( spectral index between -5 and -8) extending down to ˜ 7 keV. Thermal emission is found to dominate below ˜ 7 keV. In many other respects, microflares show properties similar to larger flares. We present single event studies of different types of x-ray microflares. RHESSI observations during quiet times (04-May 10-14; GOES level low B class) reveal a set 5 microflares (>=A Class). These microflares show power law spectra (spectral index of ˜4-8) with little or no thermal emission in the 3- ˜7 keV energy range above the nonthermal part of the spectrum. Other microflares in the same GOES class range, however, have been found which show extremely hard spectra with emission up to 50 keV (power law index ˜2). At lower energies, emission is dominated by a hot thermal component (20 MK). This work was supported by NASA contract NAS5-98033.

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