Rotational characteristics of the white-light solar corona 1965-1983

Details Rotational characteristics of the white-light solar corona 1965-1983 Rotational characteristics of the white-light solar corona 1965-1983

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...287..959f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 287, Dec. 15, 1984, p. 959-968. NSF-sponsored research.

Astronomy and Astrophysics

Astrophysics

34

Light (Visible Radiation), Solar Corona, Solar Rotation, Autocorrelation, Photosphere, Space Plasmas, Sunspots

Scientific paper

Data from the series of HAO K-coronameters located at Mauna Loa, Hawaii, are analyzed with an autocorrelation technique for the purpose of defining the variation of synodic rotation period and white-light structure persistence as a function of the solar activity cycle. The time-averaged results yield a rotation law of ω = 14.21-0.57 sin2φ degrees per day, where ω is the sidereal rotation rate at latitude φ. This is equal to the sunspot rotation rate at the equator but is much more rigid than rotational characteristics of photospheric magnetic fields or sunspots. A variation of the rotation rate is observed, with a definite dependence upon the level of solar activity.

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