Torsional oscillations in the solar corona

Details Torsional oscillations in the solar corona Torsional oscillations in the solar corona

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..615m&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 615

Astronomy and Astrophysics

Astronomy

4

Solar Corona, Solar Oscillations, Solar Rotation, Sunspots, Solar Activity, Solar Magnetic Field, Torsional Vibration, Solar Cycles

Scientific paper

The dependence of the differential rotation of the solar corona on latitude and time is investigated using observations in the Fe XIV 5303 A line from 1940 to 1992. Five bands of fast and slow rotation relative to the average value are distinguished. The bands of slow rotation arise after the reversal of the polar magnetic field of the sun and migrate toward the equator over the course of eight to 15 years along the 'butterfly' patterns of polar faculae and of the sunspots of the following cycle. The bands of fast rotation arise 5-6 years later, and also migrate toward the equator parallel to the bands of slow rotation. The fastest latitude drift of the bands was observed from 1945 to 1955 and preceded the maximum of the 19th solar activity cycle (1955-1965). The amplitude of the azimuthal component of the coronal rotation relative to the mean rotation varied within +/- 30 m/s. The equatorial drift velocity varied from 3 to 5 m/s. The latitude-time distribution of the zones with slow coronal rotation is associated with the appearance of high-latitude and middle-latitude coronal holes after the reversal of the solar polar magnetic field and during the solar activity maximum of the next sunspot cycle. The origin of the zones of anomalous rotation in the corona and their dynamics in the global activity cycle are discussed.

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