A new technique for solving Parker-type wind equations.
Abstract
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.
- Publication:
-
Journal of Computational Physics
- Pub Date:
- February 1988
- DOI:
- 10.1016/0021-9991(88)90090-3
- Bibcode:
- 1988JCoPh..74..488M
- Keywords:
-
- Computational Astrophysics;
- Cosmology;
- Stellar Mass Ejection;
- Stellar Winds;
- Differential Equations;
- Neutron Stars;
- Quasars;
- Stellar Envelopes;
- X Ray Sources;
- Astrophysics;
- Compact Objects:Mass Flow;
- Compact Objects:Stellar Winds;
- Mass Flow:Compact Objects;
- Stellar Winds:Compact Objects