Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983georl..10.1120s&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 10, Nov. 1983, p. 1120-1123.
Astronomy and Astrophysics
Astronomy
2
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.
Murakami Masaaki
Sato Takeshi
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