Astrophysics and Space Science

, Volume 108, Issue 1, pp 203–217 | Cite as

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

  • Shinpei Shibata
  • Osamu Kaburaki
Article
Received:
Revised:

Abstract

Under the purely centrifugal approximation (gravity and pressure force are neglected), stellar magnetospheres are classified into three main types of 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 illustrate this mechanism, the type II magnetosphere is taken up 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. Our model reproduces a disk-like outflow of the centrifugal wind across the magnetic field lines which are closed through the equatorial plane.

Keywords

Viscosity Magnetic Field Parameter Space Field Strength Characteristic Equation 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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Copyright information

© D. Reidel Publishing Company 1985

Authors and Affiliations

  • Shinpei Shibata
    • 1
  • Osamu Kaburaki
    • 1
  1. 1.Astronomical Institute, Faculty of ScienceTohoku UniversitySendaiJapan

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