Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...494..669m&link_type=abstract
Astronomy and Astrophysics, Volume 494, Issue 2, 2009, pp.669-675
Astronomy and Astrophysics
Astrophysics
6
Acceleration Of Particles, Shock Waves, Sun: Flares, Sun: X-Rays, Gamma Rays, Sun: Radio Radiation
Scientific paper
Context: During solar flares a large amount of energy is suddenly released and partly transferred into energetic electrons. They are of special interest since a substantial part of the energy released during a flare is deposited into the energetic electrons. RHESSI observations, e.g. of the 2003 October 28 solar event, show that 1036 electrons with energies >20 keV are typically produced per second during large flares. They are related to a power of about 1022 W. It is still an open question in which way so many electrons are accelerated up to high energies during a fraction of a second. Aims: Within the framework of the magnetic reconnection scenario, jets appear in the outflow region and can establish standing fast-mode shocks if they penetrate the surrounding plasma with super-Alfvénic speed. It is our aim to show that this shock can be the source of the energetic electrons produced during flares. Methods: The electrons are regarded as energized by shock drift acceleration. The process is necessarily treated in a fully relativistic manner. The resulting distribution function of accelerated electrons is a loss-cone one and it allows to calculate the differential electron flux, which can be compared with RHESSI. Results: The theoretically obtained fluxes of energetic electrons agree with the observed ones as demonstrated for the 2003 October 28 solar event.
Aurass Henry
Mann Gottfried
Warmuth Alexander
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