Solar X-ray Bursts and Electron Acceleration Down to 8 keV

Details Solar X-ray Bursts and Electron Acceleration Down to 8 keV Solar X-ray Bursts and Electron Acceleration Down to 8 keV

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp52b02l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP52B-02

Physics

7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

In two days typical of solar maximum (October 1-2, 1991), the Compton Gamma Ray Observatory (CGRO) Burst and Transient Source Experiment (BATSE) Spectroscopy Detectors (SPECs) observed > ~5 solar X-ray bursts per hour above 8keV [8-13 keV flux > 0.4 (cm2-s-keV)-1]. Only ~1/3 of these were detected above 25 keV [25-59 keV flux > 1.7x10-3 (cm2-s-keV)-1] by the BATSE Large Area Detectors (LADs). Most of the >8keV bursts are impulsive, and occur on the most rapid rise of the GOES thermal soft X-ray (SXR) burst. Assuming a power law spectrum (dJ/dE ~ E-g), the ratio of 8-13 keV to >13 keV flux for the impulsive bursts fit g = 3-7, similar to solar HXR bursts observed above 20 keV. More than half of the bursts that should be detected by the LADs if the power law extends to high energies are not detected, suggesting that the spectrum steepens or cuts off above ~25 keV. The burst occurrence frequency varies with energy W in >8 keV electrons as dn/dW ~W-1.6 above W ~ 1029 ergs. This power law is consistent with the distribution of energy released in small active region transient brightenings (detected in thermal emission by the Yohkoh Soft X-ray Telescope) from ~1025 to 1029 ergs. These findings suggest that the acceleration of electrons occurs for essentially all impulsive energy releases, but may only be detectable at low energies < ~10 keV in smaller releases.

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