Visibility and rate of coronal mass ejections

Details Visibility and rate of coronal mass ejections Visibility and rate of coronal mass ejections

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...98..369s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 98, Aug. 1985, p. 369-378.

Physics

12

Solar Corona, Solar Flares, Solar Radio Bursts, Stellar Mass Ejection, Type 2 Bursts, Visibility

Scientific paper

Two thirds of the Hα flares associated in time and position with coronal mass ejections (CME) observed by the Coronagraph/Polarimeter (C/P) or by the coronagraph on Skylab lie within 30° of the solar limb. The high rate of CME association at the limb is interpreted here to imply: (1) Most type II flares (at least 80%) are physically associated with mass motion in the corona (although about half of CME flares lack type II bursts). (2) The longitude window, centered on the plane of the sky, within which C/P and Skylab coronagraphs detect CME has halfwidth of 20° to 30°. (3) CME observed at polar position angles are unlikely to be flare associated. (4) The total number of mass ejections must be considerably greater than the number detected. The ratio of total number to observed number is estimated to be between 2 and 3, and the total occurence frequency of coronal mass ejections at solar-cycle maximum to be comparable to that of flares of importance 1.

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