The cross-section for bremsstrahlung photon emission in solar flares is in general a function of the angle θ between the incoming electron and the outgoing photon directions. Thus the electron spectrum required to produce a given pho- ton spectrum is a function of this angle, which is related to the position of the flare on the solar disk and the direction(s) of the pre-collision electrons relative to the local solar vertical. We compare mean electron flux spectra for the flare of August 21, 2002, using cross-sections for parameterized ranges of the angle θ. Implications for the shape of the mean source electron spectrum, and for the injected power in nonthermal electrons, are discussed.
Anisotropic bremsstrahlung emission and the form of regularized electron flux spectra in solar flares.
A. M. Massone;PIANA, MICHELE;
2004-01-01
Abstract
The cross-section for bremsstrahlung photon emission in solar flares is in general a function of the angle θ between the incoming electron and the outgoing photon directions. Thus the electron spectrum required to produce a given pho- ton spectrum is a function of this angle, which is related to the position of the flare on the solar disk and the direction(s) of the pre-collision electrons relative to the local solar vertical. We compare mean electron flux spectra for the flare of August 21, 2002, using cross-sections for parameterized ranges of the angle θ. Implications for the shape of the mean source electron spectrum, and for the injected power in nonthermal electrons, are discussed.
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