On the coronal source regions of U bursts - From observations with the three-frequency radioheliograph and the spectropolarimeter at Culgoora

Details On the coronal source regions of U bursts - From observations with the three-frequency radioheliograph and the spectropolarimeter at Culgoora On the coronal source regions of U bursts - From observations with the three-frequency radioheliograph and the spectropolarimeter at Culgoora

Apr 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...57..415s&link_type=abstract

Solar Physics, vol. 57, Apr. 1978, p. 415-422.

Physics

11

Circular Polarization, Magnetoionics, Solar Activity Effects, Solar Corona, Type 3 Bursts, Contours, Frequency Distribution, Plasma Waves, Polarimeters, Solar Magnetic Field, Spectroheliographs, Very High Frequencies

Scientific paper

It is generally accepted that Type III bursts are generated by electron streams traveling along open magnetic field lines for normal Type III bursts and along magnetic loops for the U bursts. The electron streams generate longitudinal plasma waves which are partially scattered into electromagnetic radiation, believed to be of the ordinary magnetoionic mode (o-mode). In the present paper, projected source positions at 43, 80, and 160 MHz and the sense and degree of circular polarization in the range from 24 to 220 MHz, as observed with the Culgoora radio heliograph and spectropolarimeter, respectively, are used to substantiate the hypothesis that metric U bursts originate in high coronal magnetic loops and to strengthen the hypothesis that U burst radiation is in the ordinary o-mode. The occasional observation of different senses of circular polarization on either side of the turning point of a U burst suggests that U-burst radiation in these cases reaches its limiting polarization at or near the source.

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