A new technique for solving the Parker-type wind equations

Details A new technique for solving the Parker-type wind equations A new technique for solving the Parker-type wind equations

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jcoph..74..488m&link_type=abstract

Journal of Computational Physics (ISSN 0021-9991), vol. 74, Feb. 1988, p. 488-492.

Statistics

Computation

4

Computational Astrophysics, Cosmology, Stellar Mass Ejection, Stellar Winds, Differential Equations, Neutron Stars, Quasars, Stellar Envelopes, X Ray Sources

Scientific paper

Substitution of the novel function Phi for velocity, as one of the dependent variables in Parker-type solar wind equations, removes the critical point, and therefore the numerical difficulties encountered, from the set of coupled differential wind equations. The method has already been successfully used in a study of radiatively-driven mass loss from the surface of X-ray bursting neutron stars. The present technique for solving the equations of time-independent mass loss can be useful in similar applications.

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