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- W2493914047 abstract "The hot corona surrounding a late-type star spontaneously expands as a thermo-centrifugal wind. In a system symmetric about the rotation axis, the shear generated through angular momentum conservation by the wind gas, twists stellar magnetic field lines, generating torques that brake the star's rotation by transfer of angular momentum to the wind. Within the wind zone is a non-expanding ‘dead zone’ in co-rotation with the star. The angular momentum carried jointly by the wind gas and associated Maxwell stresses is equivalent to having the gas kept in co-rotation with the star out to the surface, where the gas reaches the local Alfvèn speed — ‘effective co-rotation’. If the magnetic axis is oblique to the rotation axis, there is also a precessional torque, tending to alter the obliquity angle. An analogous relativistic centrifugal wind is relevant to the magnetohydrodynamics of neutron stars, active galactic nuclei, and black holes." @default.
- W2493914047 created "2016-08-23" @default.
- W2493914047 creator A5056206522 @default.
- W2493914047 date "2003-06-05" @default.
- W2493914047 modified "2023-09-23" @default.
- W2493914047 title "Magnetic Braking of Stars by Winds" @default.
- W2493914047 doi "https://doi.org/10.1093/acprof:oso/9780198526728.003.0007" @default.
- W2493914047 hasPublicationYear "2003" @default.
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