Observations of coronal structure during sunspot maximum

Details Observations of coronal structure during sunspot maximum Observations of coronal structure during sunspot maximum

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ssrv...33..219s&link_type=abstract

(Lindau Workshop on the Source Region of the Solar Wind, 9th, Lindau, West Germany, Nov. 1981.) Space Science Reviews, vol. 33,

Computer Science

25

Coronal Holes, Solar Corona, Sunspots, Coronagraphs, Coronal Loops, Magnetic Measurement, Stellar Mass Ejection

Scientific paper

Observations of coronal holes and coronal transients made between 1979 and 1981, near the most recent sunspot maximum, are reported. Comparison of He I 10830-A images and photospheric magnetograms obtained almost daily since 1974 at Kitt Peak indicates that, after July 31, 1978, the average magnetic field strength and magnetic flux at the base of the coronal holes increased by a factor of 3.1, from 4.1 to 11.9 G and 1.6 to 5.0 x 10 to the 20th sq cm, respectively, while the areas of the measured holes changed by a factor of only 1.1. Observations made by the NRL earth-orbiting coronagraph since March 28, 1979, have revealed 495 mass ejections on a time scale of a few hours or less and 332 additional events of longer time scale during the parts of 1979, 1980 and 1981 for which data is available, corresponding to a rate of at least two a day. Of the 495 primary transients, at least 151 had a characteristic spike structure, while 55 have been classified as big loops and 9 as quadrant fillers. Intensity changes in the coronagraph field of view were also present following the apparent collision of comet Howard-Koomen-Michels 1979 XI with the sun.

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