Pressure distribution at the inner boundary of an astropause caused by a compressible stellar wind

Details Pressure distribution at the inner boundary of an astropause caused by a compressible stellar wind Pressure distribution at the inner boundary of an astropause caused by a compressible stellar wind

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...118...57f&link_type=abstract

Astronomy and Astrophysics, vol. 118, no. 1, Feb. 1983, p. 57-65. Research sponsored by the Deutsche Forschungsgemeinschaft.

Statistics

Computation

18

Astronomical Models, Interstellar Matter, Plasma Interactions, Stellar Winds, Computational Fluid Dynamics, Flow Geometry, Magnetohydrodynamic Flow, Pressure Distribution, Subsonic Flow

Scientific paper

An investigation is undertaken of the free contact discontinuity surfaces between two counterstreaming hydrodynamic plasmas, with attention to two aspects of the interaction region between the interstellar medium and the stellar winds of stars moving relative to it: (1) the treatment of the interstellar medium as a magnetized plasma, relative to which the motion of the stellar obstacle is likely to be sub-Alfvenic, and (2) the description of both the interstellar medium and the stellar wind as compressible plasma flows. The expressions derived for the gradient of the inclination angle between streamlines and the axis of symmetry allow the numerical construction of the total hydrodynamic flow field, if the geometry of a surface tangential to the flow is known. Pressures and flow velocities are calculated for the stellar wind plasma at astropause surfaces of an ellipsoidal shape.

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