HR: 0800h
AN: SH22A-0849    [Abstracts]
TI: RHESSI Hard X-ray Microflare Statistics
AU: * Christe, S
EM: schriste@ssl.berkeley.edu
AF: Physics Department, U.C. Berkeley, Berkeley, CA 94720,
AU: * Christe, S
EM: schriste@ssl.berkeley.edu
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AU: Hannah, I
EM: hannah@ssl.berkeley.edu
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AU: Hurford, G
EM: hurford@ssl.berkeley
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AU: McTiernan, J
EM: jimm@ssl.berkeley.edu
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AU: Lin, R
EM: rlin@ssl.berkeley.edu
AF: Physics Department, U.C. Berkeley, Berkeley, CA 94720,
AU: Lin, R
EM: rlin@ssl.berkeley.edu
AF: Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720,
AB: We present the first in-depth statistical survey of all X-ray microflares observed by RHESSI between March 2002 and March 2007, a total of 25,705 events. These microflares were found using a new flare-finding algorithm designed to search the 6--12~keV count rate when RHESSIs full sensitivity was available in order to find the smallest events. These microflares are small flares, from low GOES C Class to below A Class (background subtracted) and associated with active regions. Each microflare is automatically analyzed at the peak time of the 6--12~keV emission. Spectral parameters are determined both by considering ratios between energy channels and by forward fitting a thermal plus non-thermal model. Flare images are created using back-projection and centroids and by forward fitting the complex visibilities. The combination of imaging and spectral parameters allow for the first time analysis of the thermal and non-thermal energy at the peak time of these microflares.
DE: 7509 Corona
DE: 7519 Flares
DE: 7554 X-rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting