The formation of a standing shock in a polytropic solar wind model within 1-10 RS

Details The formation of a standing shock in a polytropic solar wind model within 1-10 RS The formation of a standing shock in a polytropic solar wind model within 1-10 RS

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90..199h&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, Jan. 1, 1985, p. 199-204.

Statistics

Computation

10

Computational Astrophysics, Shock Waves, Solar Wind, Equations Of Motion, Mathematical Models, Polytropic Processes, Solar Corona, Subsonic Flow, Wind Velocity

Scientific paper

The author shows how a one-fluid polytropic solar wind model exhibits properties similar to an isothermal wind when localized momentum addition and/or rapid area divergence produce multiple critical points in the flow. In particular, it is shown that when the sonic transition in the flow occurs closer to the coronal base, multiple steady solutions can exist. These multiple steady solutions consist of a continuous solution passing through the innermost critical point and other steady solutions involving a steady shock transition. By following the temporal evolution of the solar wind from a steady state with one critical point to a steady state with three critical points, the author shows that a standing shock solution is more likely to develop than a continuous solution when momentum deposition occurs close to the coronal base and the equation of motion admits multiple steady solutions. This result is particularly relevant to the solar wind when momentum deposition occurs as a result of a rapidly diverging coronal hole geometry.

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