Quasisteady gas flow from solar active regions, and the relationship of coronal holes

Details Quasisteady gas flow from solar active regions, and the relationship of coronal holes Quasisteady gas flow from solar active regions, and the relationship of coronal holes

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980azh....57..225m&link_type=abstract

(Astronomicheskii Zhurnal, vol. 57, Mar.-Apr. 1980, p. 225-236.) Soviet Astronomy, vol. 24, Mar.-Apr. 1980, p. 133-139. Transla

Astronomy and Astrophysics

Astronomy

2

Coronal Holes, Gas Flow, Solar Activity, Solar Corpuscular Radiation, Unsteady Flow, Solar Corona, Solar Flares

Scientific paper

The problem of the origin of the quasisteady corpuscular flow from active regions on the sun is discussed. In certain cases an active region is preceded on the solar disk by a coronal hole, with a relatively undisturbed surface area in between. This configuration, as illustrated by a diagram, can explain the 'cone of avoidance' effect. However, active regions often occur in the absence of perceptible coronal holes; the 'left hand' maximum L in the curve for the geomagnetic disturbance index as a function of time relative to meridian transit of plages should then be quite weak. These facts lend support to the author's previous claim that active regions are actually sources of quasisteady corpusuclar radiation. Numerous studies indicate that active regions with enhanced and relatively continuous flare activity are often sources of quasisteady gas streaming at comparatively high velocities. Accordingly, it is here proposed that the outflow of gas from ordinary quiescent active regions and from active regions with heightened flare activy has a common origin.

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