The magnetic and fluid environment of an ellipsoidal circumstellar plasma cavity

Details The magnetic and fluid environment of an ellipsoidal circumstellar plasma cavity The magnetic and fluid environment of an ellipsoidal circumstellar plasma cavity

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.202..735n&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 202, Feb. 1983, p. 735-752. Research sponsored by the Deutsche Forschun

Astronomy and Astrophysics

Astronomy

26

Cosmic Plasma, Interstellar Matter, Magnetohydrodynamic Flow, Stellar Magnetic Fields, Stellar Models, Stellar Winds, Ellipsoids, Plasma Diffusion, Pressure Distribution, Stellar Envelopes, Velocity Distribution

Scientific paper

The contact discontinuity surface separating a stellar wind cavity from the external magnetized and ionized interstellar plasma, or astropause, is modelled by a triaxial ellipsoid. It is argued that such a surface is likely to be closed due to the fact that the stellar wind plasma leaves the inner cavity via diffusion along the strong magnetic field gradients in the area surrounding the astropause. General solutions are obtained for the potential of the outer flow vector and magnetic field under the condition that these vectors are tangential to the astropause surface and are identical to the undisturbed interstellar vectors far from the star. The Laplacian differential equation for these conditions is solved by introducing specifically adapted ellipsoidal coordinates that permit factorization of the potential function given in terms of Weierstrass's omega and zeta functions. Specific solutions for prolate, oblate, and spherically degenerate ellipsoids are generated and discussed. The vector fields parallel and perpendicular to the main axis of the ellipsoid are shown, and the pressure distribution over the astropause is presented.

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