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- W2073676192 abstract "We present numerical solutions for axisymmetric thermo-centrifugal winds with a dipole magnetic flux distribution on the stellar surface. Parameters of the models are chosen to be those typical for the Sun, except for the angular velocity Ω 0 , which is increased to up to 60 times the solar value. The dipole moment is not increased with Ω 0 , but is kept constant. The value of β of the plasma is about unity on the stellar surface, and the range of the ratio Ω 0 ω#58 A /C s is 0-2.6, where ω#58 A is the equatorial radius of the Alfven surface and C s is the sound velocity. As the value of Ω 0 is increased to more than about 10 times the solar value, the centrifugal (electromagnetic) driving force becomes comparable with the thermal driving force, and the meridional structure of the wind is then strongly influenced by the electromagnetic force (the thermo-centrifugal wind)" @default.
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- W2073676192 date "1993-06-15" @default.
- W2073676192 modified "2023-10-14" @default.
- W2073676192 title "Thermo-centrifugal wind from a rotating magnetic dipole" @default.
- W2073676192 doi "https://doi.org/10.1093/mnras/262.4.936" @default.
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