Dynamic behaviour of the K-corona above a type I radio source

Details Dynamic behaviour of the K-corona above a type I radio source Dynamic behaviour of the K-corona above a type I radio source

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...89...63d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 89, Nov. 1983, p. 63-76. Research sponsored by the Commonwealth Scientific and Industrial R

Astronomy and Astrophysics

Astronomy

3

Coronagraphs, Radio Sources (Astronomy), Solar Corona, Solar Radio Emission, Brightness Distribution, Dynamic Response, Image Enhancement, Polarimetry, Spaceborne Astronomy

Scientific paper

Coronagraph images can be greatly enhanced by subtracting from the brightness of each picture point, the running median brightness over a square surrounding each picture point. The application of this technique to coronal analysis appears to be new. After such enhancement, images recorded by the SMM Coronagraph/Polarimeter reveal a coronal transient with previously undescribed characteristics. The transient began with bright ejecta moving up pre-existing rays and weaker, more diffuse, mass injection in the area between rays. At the sudden onset of this mass ejection the rays began to move apart from one another: during the ensuing 22 hr the separation of one pair of rays increased by 37 deg of latitude. Towards the end of the event these moving rays looked much like the legs of previously described loop transients. A type I radio source lay close to the center of symmetry of the transient.

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