Magnetorotational instability in Ap star envelopes

Details Magnetorotational instability in Ap star envelopes Magnetorotational instability in Ap star envelopes

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..224..103a&link_type=abstract

The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004. Edited by J. Zverko, J. Ziznovsky, S.J. Adelman, and W.W. Weiss,

Physics

2

Mhd, Instabilities, Stars: Rotation.

Scientific paper

The rotational evolution of the radiative zone of magnetic Ap stars is investigated with numerical simulations. An angular-velocity profile decreasing with axis distance in combination with a magnetic field leads to a magnetorotational instability. The resulting flows efficiently transport angular momentum outwards. The corresponding decay of angular-velocity gradients in the radiative zone is estimated to take about 10-100 million years.

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