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Magnetic acceleration of winds from solar-type starsThe spin-down of solar type stars (F5 V to G3 V) is generally ascribed to the outflow of magnetized plasma in the form of a wind. Magnetically coupled stellar winds are thought to provide the dominant mechanism for angular momentum loss over the entire main-sequence lifetime of stars possessing hydrogen convective zones. The associated loss in rotational kinetic energy can strongly affect the energetics of winds emanating from such stars, for sufficiently high rotation rates and magnetic field strengths. In the present paper, an attempt is made to describe qualitatively how MHD plasma outflow from a rotating star adjusts itself to a broad range of stellar conditions, including fast, intermediate, and slow magnetic rotator configurations. Using the Weber and Davis (1967) model of MHD winds, it is shown that the magnetic deceleration of an MHD wind is of importance when the loss of rotational kinetic energy due to magnetic braking exceeds the energy flux due to thermal processes alone.
Document ID
19770033168
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Belcher, J. W.
(Massachusetts Inst. of Tech. Cambridge, MA, United States)
Macgregor, K. B.
(MIT Cambridge, Mass., United States)
Date Acquired
August 9, 2013
Publication Date
December 1, 1976
Publication Information
Publication: Astrophysical Journal
Volume: 210
Subject Category
Astrophysics
Accession Number
77A16020
Funding Number(s)
CONTRACT_GRANT: NGL-22-009-015
Distribution Limits
Public
Copyright
Other

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