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Spin-Down of Solar-Type Stars with Internal Magnetic Fields

Published online by Cambridge University Press:  12 April 2016

Paul Charbonneau  and
Keith B. Macgregor
Paul Charbonneau
Affiliation:
High Altitude Observatory, NCAR, 1P.O. Box 3000, Boulder, CO 80307, U.S.A.
Keith B. Macgregor
Affiliation:
High Altitude Observatory, NCAR, 1P.O. Box 3000, Boulder, CO 80307, U.S.A.

Abstract

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We present a selection of results from a large set of numerical simulations of the spin-down of a solar-type star containing a large scale magnetic field in its radiative interior. Our computations are dynamical, in that they take into account both the generation of the toroidal component by the wind-induced shear endits back-reaction on the azimuthal flow. Our results demonstrate the existence of classes of internal magnetic fields that can accomodate rapid spin-down near the ZAMS, and yield weak internal differential rotation by the solar age.

Keywords

RotationMagnetic Fields.
Type
V. The changing interior
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 464 - 468
Copyright
Copyright © Astronomical Society of the Pacific 1993

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