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Radio Physics and Radio Astronomy

ISSN 印刷: 2152-274X
ISSN オンライン: 2152-2758

Archives: Volume 1, 2010 to Volume 3, 2012

Radio Physics and Radio Astronomy

DOI: 10.1615/RadioPhysicsRadioAstronomy.v3.i3.30
pages 205-213

PROPAGATION OF TYPE III SOLAR BURSTS RADIO EMISSION THROUGH THE CORONA. 1. TIME PROFILE

B. P. Rutkevych
Institute of Radio Astronomy, National Academy of Sciences of Ukraine
V. N. Melnik
Institute of Radio Astronomy, National Academy of Sciences of Ukraine

要約

The propagation of electromagnetic waves in the coronal plasma, from the area of generation toward an observer, is considered based on the generally accepted plasma theory of type III burst generation. Special attention is given to the increase in the group velocity of the electromagnetic waves, arising from the variation in the plasma density away from the Sun. An analytic formula for the wave's group velocity as function of the generation area coordinate and of separation from that has been derived. The formula is used to analyze the group delay of the waves within two models of the corona. Taking into account the spatial size of the electron beam, it has become possible to obtain representations for the time profile of the electromagnetic radiation. A fine-structured electron beam has been considered. The radiation profile from such a beam can be shown to resemble closely the observed profile of type III bursts with a fine structure. Also, a spherical beam of a monotonically increasing radius is considered, and the dynamic spectrum of type III bursts is derived. The burst duration has been evaluated over a broad frequency range.


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