A self-consistent model of the magnetosphere with centrifugal wind. I

Details A self-consistent model of the magnetosphere with centrifugal wind. I A self-consistent model of the magnetosphere with centrifugal wind. I

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.108..203s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 108, no. 1, Jan. 1985, p. 203-217.

Astronomy and Astrophysics

Astrophysics

7

Centrifugal Force, Self Consistent Fields, Stellar Magnetic Fields, Stellar Magnetospheres, Stellar Models, Stellar Winds, Corotation, Lines Of Force, Rotating Plasmas

Scientific paper

Under the purely centrifugal approximation (gravity and pressure force are neglected), stellar magnetospheres are classified into three main types having different physical properties in the two-dimensional parameter space. They are characterized essentially by the strength of the magnetic field and the plasma density at the base of the magnetosphere. Among the three types, the type II magnetosphere has moderate surface densities for a given field strength and is expected to possess a centrifugal wind blowing across the magnetic field lines without affecting them appreciably. Such a situation may be realized through a modification of the electric field from that under the ideal-MHD condition, owing to the inertia of a plasma. In order to ilustrate this mechanism, the type II magnetosphere is used for a numerical simulation. The effect of artificial viscosity is avoided by integrating the characteristic equations for both components of the plasma instead of solving the fluid equations directly. The model reproduces a disklike outflow of the centrifugal wind across the magnetic field lines, which are closed through the equatorial plane.

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