Three frequency observations of a moving type IV burst at the limb

Details Three frequency observations of a moving type IV burst at the limb Three frequency observations of a moving type IV burst at the limb

Sep 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977pasau...3..159n&link_type=abstract

(Astronomical Society of Australia, Annual General Meeting, 11th, Clayton, Victoria, Australia, May 30-June 1, 1977.) Astronomic

Astronomy and Astrophysics

Astronomy

5

Radio Spectra, Solar Limb, Spectroheliographs, Type 4 Bursts, Brightness Temperature, Circular Polarization, Radio Sources (Astronomy), Solar Radio Bursts, Stellar Models, Synchrotron Radiation, Visual Observation

Scientific paper

Observations of a moving type IV (IVM) burst above the west limb of the sun with a two-dimensional radioheliograph operating at frequencies of 43, 80, and 160 MHz are reported. The observations are summarized in plots showing the observed distances of the centroids of IVM sources from the center of the sun, the half-power widths of the strongest IVM sources, the peak brightness temperatures of the IVM sources, and the degrees of circular polarization. Significant features of the observations are discussed, the data are compared with existing models of IVM bursts, a modified synchrotron model is outlined, and the density of the IVM plasma cloud is evaluated. It is concluded that: (1) synchrotron emission from mildly relativistic particles seems to be a satisfactory mechanism to account for the radiation from IVM bursts; (2) the emission spectrum depends strongly on the location in the source where the radiation originates; (3) a Gaussian or a high-index power-law energy spectrum is required to reproduce the steepness of the observed spectra; (4) most of the plasma cloud is less dense than the surrounding corona; and (5) the cloud as a whole may be buoyant.

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