Statistics – Computation
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...226..209k&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 226, no. 1, Dec. 1989, p. 209-214. Research supported by ASTRON.
Statistics
Computation
7
Stellar Coronas, Stellar Mass Accretion, Stellar Models, Time Dependence, Computational Astrophysics, Interstellar Matter, Solar Corona, Stellar Winds
Scientific paper
Models of stationary extended coronae are presented for various values of the interstellar density. These calculations have been performed with the implicit time-dependent numerical method developed by Korevaar and Van Leer (1988). If the interstellar density is sufficiently low, the coronal gas expands through the Parker critical point to supersonic velocities. An increase in the interstellar density moves the interstellar shock closer to the star. When it comes closer than the critical point, the flow changes to a breeze solution that is subsonic everywhere. A further increase in the interstellar density reverses the flow. First an accretion breeze solution is found and then an inflow with a stationary accretion shock. This is the first numerical calculation of the complete set of stationary stellar wind solutions in spherical symmetry with boundary conditions specified at the stellar surface and at infinity, including the solutions with an interstellar shock or an accretion shock.
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