HR: 11:15h
AN: SP42A-04    [Abstracts]
TI: Microflare Statistics and Frequency Distribution
AU: * Christe, S D
EM: schriste@ssl.berkeley.edu
AF: Physics Dept., University of California, Berkeley, CA 94720 United States
AU: * Christe, S D
EM: schriste@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 United States
AU: Hannah, I
EM: iain@astro.gla.ac.uk
AF: Physics Dept., University of California, Berkeley, CA 94720 United States
AU: Rauscher, E
EM: emily_r@ssl.berkeley.edu
AF: Physics Dept., University of California, Berkeley, CA 94720 United States
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 United States
AU: McTiernan, J
EM: jimm@apollo.ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 United States
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Physics Dept., University of California, Berkeley, CA 94720 United States
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 United States
AB: RHESSI is uniquely suited to observe solar microflares due to its unique sensitivity in the 3-15 keV energy range (up to ~100 times better than previous solar instruments). As such, it provides new information on these low level transients. Initial results (Krucker et al 2002, Benz & Grigis 2002) suggest that microflares are different from larger flares. They are more often associated with steep nonthermal spectra (power law index -5 to -7). In this study, we present microflare statistics from times of low activity. A list of microflares was created by applying the standard RHESSI flare-finding algorithm to the lower 6-12 keV energy range (~10,000 events). Imaging was used in order to obtain positions of solar events and reject non-solar events. These solar events were then each spectrally analyzed. We present microflare statistics, including active region productivity, and the microflare frequency distribution. This work was supported by NASA contract NAS5-98033.
DE: 7509 Corona
DE: 7519 Flares
DE: 7537 Solar and stellar variability
DE: 7554 X rays, gamma rays, and neutrinos
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly