The synchrotron-maser theory of type II solar radio emission processes - The physical model and generation mechanism

Details The synchrotron-maser theory of type II solar radio emission processes - The physical model and generation mechanism The synchrotron-maser theory of type II solar radio emission processes - The physical model and generation mechanism

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...309..392w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 1, 1986, p. 392-401.

Astronomy and Astrophysics

Astrophysics

20

Magnetohydrodynamic Stability, Masers, Synchrotron Radiation, Type 2 Bursts, Coronal Loops, Electron Acceleration, Magnetic Mirrors, Shock Waves, Solar Magnetic Field

Scientific paper

A theory is proposed to explain the generation mechanism of type II solar radio bursts. It is suggested that the shock wave formed at the leading edge of a coronal transient can accelerate electrons. Because of the nature of the acceleration process, the energized electrons can possess a 'hollow-beam' type distribution function. When the electron beam propagates along the ambient magnetic field to lower altitudes and attains larger pitch angles, a synchrotron-maser instability can set in. This instability leads to the amplification of unpolarized or weakly polarized radiation. The present discussion incorporates a model which describes the ambient magnetic field and background plasma by means of MHD simulation. The potential emission regions may be located approximately, according to the time-dependent MHD simulation. Since the average local plasma frequency in the source region can be evaluated from the MHD model, the frequent drift associated with the radiation may be estimated. The result seems to be in good agreement with that derived from observations.

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