Coronal evolution during the sunspot cycle - Coronal holes observed with the Mauna Loa K-coronameters

Details Coronal evolution during the sunspot cycle - Coronal holes observed with the Mauna Loa K-coronameters Coronal evolution during the sunspot cycle - Coronal holes observed with the Mauna Loa K-coronameters

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981jgr....86.2079h&link_type=abstract

Journal of Geophysical Research, vol. 86, Apr. 1, 1981, p. 2079-2094.

Astronomy and Astrophysics

Astronomy

65

Coronal Holes, Solar Corona, Solar Magnetic Field, Sunspot Cycle, Sunspots, Astronomical Maps, Coronagraphs, Equatorial Regions, Polar Regions, Solar Eclipses, Solar Wind

Scientific paper

The white-light corona was observed regularly at the Mauna Loa Observatory during the years 1965-1967 and 1969-1978. Display of the measured polarization brightness in the form of synoptic maps permits the identification of large coronal holes and the study of their slow evolution during the sunspot cycle. The polar coronal holes were clearly seen to shrink in size during the ascending phase of cycle 20 (1965-1967), to be absent during a two-year period (1969-1970) just after sunspot maximum, to reappear near the end of 1970, and to remain as prominent features of the corona for the years 1971-1978. During the sunspot maximum epoch the corona was dominated by mid-latitude holes, elongated in the direction parallel to the solar equator. Large equatorial holes or equatorward extensions of the polar holes were observed during the ascending, maximum, and descending phases of cycle 20 and appear to be sources of solar wind streams with maximum speeds over 6000 km/s at all of these epochs. The lifetimes of these holes and streams were greatest during the descending phase of the cycle, or in 1974-1975.

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