Magnetic acceleration of winds from solar-type stars

Details Magnetic acceleration of winds from solar-type stars Magnetic acceleration of winds from solar-type stars

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...210..498b&link_type=abstract

Astrophysical Journal, vol. 210, Dec. 1, 1976, pt. 1, p. 498-507.

Astronomy and Astrophysics

Astrophysics

122

Angular Momentum, Magnetic Effects, Mass Transfer, Stellar Rotation, Stellar Winds, Convection, Hydrogen, Magnetohydrodynamic Stability, Momentum Transfer, Nonrelativistic Mechanics, Particle Acceleration, Stellar Magnetic Fields

Scientific paper

The 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.

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