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The Localization of Particle Acceleration Sites in Solar Flares and CMEs View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2005-07-20 17:54

We review the particular aspect of localizing particle acceleration sites in solar flares and coronal mass ejections (CMEs). Depending on the magnetic field configuration at the particle acceleration site, distinctly different radiation signatures are produced: (1) If accelerated along compact closed magnetic field lines, they precipitate to the solar chromosphere and produce hard X-rays, gamma rays, soft X-rays, and EUV emission; (2) if injected into large-scale closed magnetic field structures, they remain temporarily confined (or trapped) and produce gyrosynchrotron emission in radio and bremsstrahlung in soft X-rays; (3) if accelerated along open field lines they produce beam-driven plasma emission with a metric starting frequency; and (4) if accelerated in a propagating CME shock, they can escape into interplanetary space and produce beam-driven plasma emission with a decametric starting frequency. The latter two groups can be geo-effective if suitably connected to the solar west side. Particle acceleration sites can often be localized by modeling the magnetic topology from images in different wavelengths and by measuring the particle velocity dispersion from time-of-flight delays.

Authors: Markus J. Aschwanden
Projects: Yohkoh-HXT,Yohkoh-SXT,TRACE

Publication Status: Space Science Reviews; and Space Science Series of ISSI, Proc. of ISSI Workshop - Solar Dynamics and its Effects on the Heliosph
Last Modified: 2005-07-20 17:54
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