Journal
ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS
Volume 35, Issue 1, Pages 57-69Publisher
MAIK NAUKA/INTERPERIODICA/SPRINGER
DOI: 10.1134/S1063773709010071
Keywords
Sun; solar flares; magnetic reconnection; particle acceleration; X-ray emission
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The problem of particle acceleration in collapsing magnetic traps in the solar corona has been solved by taking into account the particle scattering and braking in the high-temperature plasma of solar flares. The Coulomb collisions are shown to be weak in traps with lifetimes t(l) < 10 s and strong for t(l) > 100 s. In the approximation of strong collisions, collapsing magnetic traps are capable of confining up to 20% of the injected particles in the corona for a long time. In the collisionless approximation, this value exceeds 90%. The question about the observational manifestations of collisions is examined. For collision times comparable to t(l), the electron spectrum at energies above 10 keV is shown to be a double-power-law one. Such spectra were found by the RHESSI satellite in flares.
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