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Frequency Distributions of Solar Microwave Burst Parameters View all abstracts by submitter

Jeongwoo Lee   Submitted: 2008-12-17 12:23

Microwave bursts during solar flares are known to be sensitive to high energy electrons and magnetic field, both of which are important ingredients of solar flare physics. This paper presents such information derived from the microwave bursts of the 412 flares that were measured with the Owens Valley Solar Array (OVSA). We assumed that these bursts are predominantly due to gyrosynchrotron radiation by nonthermal electrons in a single power-law energy distribution to use the simplified formulae for gyrosynchrotron radiation in the data analysis. A second major assumption was that statistical properties of flare electrons derived from this microwave database should agree with an earlier result based on the Hard X-Ray Burst Spectrometer (HXRBS) on SMM. Magnetic field information was obtained in the form of a scaling law between average magnetic field and total source area, which turns out to a narrow distribution around ~400 gauss. The derived nonthermal electron energy is related to the peak flux, peak frequency, and spectral index, through a multi-step regression fit, which can be used for a quick estimate for the nonthermal electron energy from spatially-integrated microwave spectral observations.

Authors: Jeongwoo Lee, Gelu M. Nita, and Dale E. Gary
Projects: None

Publication Status: ApJ, in press
Last Modified: 2008-12-17 12:51
Go to main E-Print page  First 3D Reconstructions of Coronal Loops with the STEREO A+B Spacecraft: III. Instant Stereoscopic Tomography of Active Regions  The Kinematics of Coronal Mass Ejections using Multiscale Methods  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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