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Magnetorotational instability in Ap star envelopes

Published online by Cambridge University Press:  02 March 2005

Reiner Arlt
Reiner Arlt
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: rarlt@aip.de
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Abstract

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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.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

MHDinstabilitiesstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 103 - 108
Copyright
© 2004 International Astronomical Union