Colliding winds - Interaction regions with strong heat conduction

Details Colliding winds - Interaction regions with strong heat conduction Colliding winds - Interaction regions with strong heat conduction

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..313i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 1, 1984, p. 313-318.

Statistics

Computation

4

Conductive Heat Transfer, Shock Waves, Stellar Winds, Wind Velocity, Computational Fluid Dynamics, Conservation Equations, Electron Energy, Ion Temperature, Solar Wind, Stellar Mass Ejection, Wind Direction

Scientific paper

The interaction of a fast stellar wind with a slower wind from previous mass loss gives rise to a region of hot shocked gas. Self-similar solutions are obtained for the interaction region under the assumptions of constant mass loss rate and wind velocity for the two winds, conservation of energy in the shocked region, and either isothermal electrons and adiabatic ions or isothermal electrons and ions in the shocked region. The isothermal assumption is intended to show the effects of strong heat conduction. The solutions have no heat conduction through the shock waves and assume that the electron and ion temperatures are equilibrated in the shock waves. The one-temperature isothermal solutions have nearly constant density through the shocked region, while the two-temperature solutions are intermediate between the one-temperature adiabatic and isothermal solutions. In the two-temperature solutions, the ion temperature goes to zero at the point where the gas comoves with the shocked region and the density peaks at this point. The solutions may qualitatively describe the effects of heat conduction on interaction regions in the solar wind. It will be important to determine whether the assumption of no thermal waves outside the shocked region applies to shock waves in the solar wind.

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