Electron acceleration to high energies at quasi-parallel shock waves in the solar corona

Details Electron acceleration to high energies at quasi-parallel shock waves in the solar corona Electron acceleration to high energies at quasi-parallel shock waves in the solar corona

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...28m&link_type=abstract

Observatorium für Solare Radioastronomie, International Solar Wind 8 Conference, p. 28

Astronomy and Astrophysics

Astronomy

Electron Acceleration, Magnetic Mirrors, Type 2 Bursts, Solar Wind, Magnetic Field Configurations, Relativistic Particles, Shock Waves, Relativistic Velocity, Radio Spectra, Solar Magnetic Field, Electron Energy, Solar Wind Velocity

Scientific paper

In the solar corona shock waves are generated by flares and/or coronal mass ejections. They manifest themselves in solar type 2 radio bursts appearing as emission stripes with a slow drift from high to low frequencies in dynamic radio spectra. Their nonthermal radio emission indicates that electrons are accelerated to suprathermal and/or relativistic velocities at these shocks. As well known by extraterrestrial in-situ measurements supercritical, quasi-parallel, collisionless shocks are accompanied by so-called SLAMS (short large amplitude magnetic field structures). These SLAMS can act as strong magnetic mirrors, at which charged particles can be reflected and accelerated. Thus, thermal electrons gain energy due to multiple reflections between two SLAMS and reach suprathermal and relativistic velocities. This mechanism of accelerating electrons is discussed for circumstances in the solar corona and may be responsible for the so-called 'herringbones' observed in solar type 2 radio bursts.

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