Spin-down of rapidly rotating, convective stars

Details Spin-down of rapidly rotating, convective stars Spin-down of rapidly rotating, convective stars

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..269t&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 2, May 15, 1992, p. 269-276.

Astronomy and Astrophysics

Astronomy

57

Accretion Disks, Cataclysmic Variables, Novae, Stellar Mass Ejection, Stellar Rotation, Stellar Winds, Angular Momentum, Convection, Dynamo Theory, Magnetohydrodynamics, Spin Dynamics, Stellar Models

Scientific paper

A model for the spindown of rapidly rotating convective stars is developed. It is assumed that rotation and convection cause a stars to rotate differentially, that differential rotation and convection generate a magnetic dynamo, that a magnetic dynamo gives rise to mass loss and a magnetically controlled stellar wind, and that such a wind results in angular momentum loss and hence stellar spindown. The model is used to show that a protostar accretion from a circumstellar disk can reach an equilibrium rotation period significantly below breakup. The derived spindown rates are consistent with those required to drive the orbital evolution of cataclysmic variables.

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