A numerical model of centrifugal wind in a rapidly rotating magnetosphere

Astronomy and Astrophysics – Astronomy

Scientific paper

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Astronomical Models, Centrifugal Force, Earth Magnetosphere, Magnetohydrodynamic Flow, Rotating Plasmas, Stellar Winds, High Pressure, Low Pressure, Plasma Density, Stellar Atmospheres, Thermal Energy

Scientific paper

The plasma flow dynamics of a rapidly rotating, axisymmetric magnetosphere is studied by means of a numerical model which emphasizes the evolution of the outward plasma flow, or centrifugal wind, and the associated conformation of the magnetosphere, for two cases: (1) a high pressure case in which the corotation speed is smaller than the magnetosonic speed, and (2) a low pressure case in which the corotation speed exceeds the magnetosonic speed beyond a certain distance. It is noted that the ability of the magnetosphere to form a disk-like structure largely depends on the magnetospheric pressure distribution, and it is confirmed that a supermagnetosonic centrifugal wind is generated beyond the critical point where the rotational energy equals the sum of the magnetic and thermal energies. These results are compared with Jovian magnetosphere observations.

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