Computer Science – Numerical Analysis
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..677z&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 2, p. 677-685
Computer Science
Numerical Analysis
14
Astronomical Models, Galactic Cosmic Rays, Interplanetary Medium, Shock Waves, Solar Wind, Algorithms, Numerical Analysis, Rankine-Hugoniot Relation
Scientific paper
The solar wind spherical flow is considered under the combined action of gas pressure, magnetic pressure and pressure of cosmic rays. The formation of the solar wind termination shock in the presence of galactic cosmic rays and of the anomalous component cosmic rays, produced at the shock, is described. Taking into account of the production efficiency, defined as the ratio of the solar wind energy flux that sinks to the cosmic ray flux to the total energy flux, leads to the modified Rankine-Hugoniot equations. The numerical solution of the set of five coupled nonlinear equations describing the system is presented. The dependence on radius of the solar wind velocity and of the cosmic ray pressure is considered in both supersonic and subsonic regions. Significant deceleration of the solar wind should be observable at a distance greater than or equal 50 AU. The dependence of the shock radius on the production efficiency epsilon is discussed. With the reasonable value of epsilon approximately equal 10% the shock is situated at r approximately 80 AU.
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