Hard X-ray Microflares down to 3~keV

Details Hard X-ray Microflares down to 3~keV Hard X-ray Microflares down to 3~keV

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh52a0484c&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH52A-0484

Other

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

Scientific paper

The excellent sensitivity, spectral and spatial resolution, and energy coverage down to 3~keV provided by the Reuven Ramaty Solar Spectroscopic Imager mission (RHESSI) allows for the first time the detailed study of the locations and the spectra of solar microflares down to 3~keV. During a one hour quiet interval (GOES soft X-ray level around B6) on May~2, 1:40-2:40UT, at least 7 microflares occurred with the largest peaking at A6 GOES level. The microflares are found to come from 4 different active regions including one behind the west limb. At 7" resolution, some events show elongated sources, while others are unresolved point sources. In the impulsive phase of the microflares, the spectra can generally be fitted best with a thermal model plus power-law above ~6-7~keV. The decay phase sometimes can be fit with a thermal only, but in some events, power-law emission is detected late in the event indicating particle acceleration after the thermal peak of the event. The power-law fits extend to below 7~keV with exponents between -5 and -8, and imply a total non-thermal electron energy content between 1026-1027 ergs. Since the total energy in non-thermal electrons is very sensitive to the value of the power-law and the energy cutoff, these observations will give us better estimates of the total energy input into the corona. Presently, microflare observations on June~26 02:20-06:10UT are being analyzed and are expected to corroborate these results.

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