Frequency of coronal transients and solar activity

Details Frequency of coronal transients and solar activity Frequency of coronal transients and solar activity

May 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976soph...48..127h&link_type=abstract

Solar Physics, vol. 48, May 1976, p. 127-135.

Physics

47

Solar Activity, Solar Corona, Sunspots, Transient Response, Coronagraphs, Frequency Measurement, Magnetic Effects, Solar Magnetic Field, Time Dependence

Scientific paper

The white light coronagraph aboard Skylab observed at least 110 coronal transients during 227 days of observations. It is shown that these transients occurred preferentially at longitudes where the sunspot number and the area times brightness index of calcium plages were high. The number of transients observed to arise from each of four quadrants in heliographic longitude, rotation by rotation, was strongly correlated with the average value of these measures of solar activity. From this it is inferred that coronal transients occur more commonly where magnetic fields are stronger, more complex, and varying more rapidly.

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