Rotation of the solar convection zone from helioseismology

Details Rotation of the solar convection zone from helioseismology Rotation of the solar convection zone from helioseismology

2006-10-31

arxiv.org/abs/astro-ph/0610942v1

Astronomy and Astrophysics

Astrophysics

12 pages, 8 figures. To appear in Proc. IAU Symposium 239: Convection in Astrophysics,eds F. Kupka, I. W. Roxburgh & K. L. Cha

Scientific paper

10.1017/S1743921307000816

Helioseismology has provided very detailed inferences about rotation of the solar interior. Within the convection zone the rotation rate roughly shares the latitudinal variation seen in the surface differential rotation. The transition to the nearly uniformly rotating radiative interior takes place in a narrow tachocline, which is likely important to the operation of the solar magnetic cycle.The convection-zone rotation displays zonal flows, regions of slightly more rapid and slow rotation, extending over much of the depth of the convection zone and converging towards the equator as the solar cycle progresses. In addition, there is some evidence for a quasi-periodic variation in rotation, with a period of around 1.3 yr, at the equator near the bottom of the convection zone.

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