An explanation for the slow and uniform rotation of the solar core

Details An explanation for the slow and uniform rotation of the solar core An explanation for the slow and uniform rotation of the solar core

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508...51a&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Physics

Solar Rotation, Mhd, Instabilities

Scientific paper

The radiative core of the Sun appears to rotate uniformly and as slowly as the surface. The young Sun was a fast rotator and fully convective in the T Tauri phase. Magnetic winds can slow down the surface of the star but viscous stresses are too small to affect the stellar core thus leading to strong differential rotation. Also convection efficiently builds up differential rotation at any time of the Sun's life, and the entire star should have exhibited a non-uniform rotation profile. As convection ceased in the core, the radiative zone is left with microscopic viscosity which cannot damp differential rotation during the life-time of the Sun. We study the question why the solar radiation zone is both a slow and uniform rotator. We present magnetohydrodynamic simulations of the decay of the differential rotation profile in the radiative core due to magnetorotational instability. Unstable modes grow fast, and resulting flows equalize the rotation profile. We estimate that the decay time of the differential rotation is about 100 million years.

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