Differential rotation of the corona of the Sun as a star

Details Differential rotation of the corona of the Sun as a star Differential rotation of the corona of the Sun as a star

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..748l&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Corona, Stellar Activity, Magnetic And Electric Fields, Polarization Of Starlight

Scientific paper

The brightness of the solar corona as a whole (limb+disk) in the green line (Fe XIV 5303 Å) is estimated from the database created by J. Sykora. This coronal index GLS (Green Line Sun) is based on observations directly. A daily set of from 1939 to 2001 is analyzed with the adaptive wavelet techniques. The method applied for the Sun is the same as it used for late-type stars. We found that the synodic rotational period for inhomogeneities in the corona can exceed the mean value up to 3-4 days during epochs of the high activity. Hence it appears that ΔΩ/<Ω> = -0.13. The slowest rotation occurs when the sign of the global magnetic dipole of the Sun changes.

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