Spatial, spectral, and polarization properties of radio emission of the 3 February, 1983 proton flare

Details Spatial, spectral, and polarization properties of radio emission of the 3 February, 1983 proton flare Spatial, spectral, and polarization properties of radio emission of the 3 February, 1983 proton flare

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..135..107b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 135, Sept. 1991, p. 107-129.

Physics

5

Polarization Characteristics, Solar Flares, Solar Protons, Solar Radio Emission, Solar Spectra, Particle Acceleration, Radio Telescopes, Siberia, Solar Activity Effects, Solar Observatories

Scientific paper

The spatial, spectral, and polarization evolutionary features of a proton flare of 2B importance observed on February 3, 1983, are analyzed comprehensively via optical and radio observations obtained by various techniques. The flare was a long-duration process (about 1.5 hr) of energy release and particle acceleration, which consecutively covered still greater regions of the active-region magnetosphere extending in both area and altitude. The cm-range showed flare precursors, i.e., quasi-periodic fluctuations of the radio flux density. As a new magnetic flux was emerging, there was restructuring of the magnetic field, resulting in a long-duration formation of coronal or postflare loops which gradually embraced the area outside the sunspots, penetrating into still greater heights of up to hundreds of thousands of kilometers above the photosphere. The magnetic field strength inside the coronal transient inferred from the zebra-structure and fiber bursts at about 110 MHz was found to be higher (1-2 G) as compared with the stationary source at the end of the flare at about 230 MHz (0.5-1 G).

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