Solar radio emission very near the plasma frequency

Details Solar radio emission very near the plasma frequency Solar radio emission very near the plasma frequency

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...270..250w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 270, July 1, 1983, p. 250-255. NSF-supported research.

Astronomy and Astrophysics

Astrophysics

3

Plasma Frequencies, Solar Corona, Solar Radio Emission, Intensity, Solar Magnetic Field, Solar Radio Bursts

Scientific paper

The propagation of signals from the solar corona emitted very near the plasma frequency is investigated. The group velocity near the plasma frequency is analyzed; near the edge of the cone of emission, the bandwidth of the escaping radiation is much smaller than the inherent bandwidth of emission. Finite burst duration is observed because of the differential delays in the various parts of the signal, even when there is no subsequent coronal scattering. A formula for the burst duration when the density gradient and magnetic field are parallel is presented. For a homogeneous corona, the burst duration is 0.1 s longer than observed. The signal can be shortened by invoking a smaller density scale height near the plasma level or letting the direction of the density gradient lie outside the cone of emission. A coronal model to account for the observations is suggested.

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