Cyclic variations in the differential rotation of the solar corona

Details Cyclic variations in the differential rotation of the solar corona Cyclic variations in the differential rotation of the solar corona

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006arep...50..312b&link_type=abstract

Astronomy Reports, vol. 50, Issue 4, p.312-324

Astronomy and Astrophysics

Astronomy

4

Pacs Numbers 96.60.P - 96.60.B

Scientific paper

The rotation of the solar corona is analyzed using the original database on the brightness of the FeXIV 530.3 nm coronal green line covering six recent activity cycles. The rate of the differential rotation of the corona depends on the cycle phase. In decay phases, there are only small differences in the rotation, which are similar to that of a rigid body. The differences are more significant (though less pronounced than in the photosphere) during rise phases, just before maxima, and sometimes at maxima. The total rate of the coronal rotation is represented as a superposition of two, i.e., fast and slow modes. The synodic period of the fast mode is approximately 27 days at the equator and varies slightly with time. This mode displays weak differences in rotation and is most pronounced in the middle of decay phases. The slow mode is manifested only at high latitudes during the rise phases of activity, and displays a mean period of 31 days. The relative contribution of each mode to the total rotational rate is determined as a function of time and heliographic latitude. These results indicate that the structure of the velocity field in the convective zone must also vary with time. This conclusion can be verified by helioseismology measurements in the near future.

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