Bimodal differential rotation of the solar corona

Details Bimodal differential rotation of the solar corona Bimodal differential rotation of the solar corona

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005coska..35..180b&link_type=abstract

Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 35, no. 3, p. 180-198.

Astronomy and Astrophysics

Astronomy

3

Solar Corona, Coronal Green Line Brightness, Differential Rotation, Two Modes Of Rotation, Helioseismology

Scientific paper

Spectral Variation Analysis (SVAN) was applied to our own database of Coronal Green Line Brightness (CGLB) covering almost six solar cycles (1939-2001) to investigate differential rotation of the solar corona. Detailed knowledge of solar rotation seems to be crucial for a better understanding of the basic mechanisms of solar activity generation. The following principal results were obtained: (a) The synodic period of coronal rotation increases from 27 days at the equator to about 29 days at the latitudes of ± 40°, displaying the less pronounced differentiality than the photospheric phenomena do. (b) Above ˜ ± 45° differentiality greatly diminishes and the rotation displays actually rigid character (with the period of about 29.5 days) up to polar regions. (c) The total corona rotation may be expressed as a sum of two modes, the faster one with period of 27 days (slightly increasing towards the higher latitudes), and the slow one with the period of about 30.5 days; the relative contribution of these modes to the total rotation rate is estimated in dependence on latitude. A short comment on relation of our findings with the latest achievements of helioseismology is given.

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