A simple one-dimensional Cartesian solution of the magnetohydrodynamic equations describing the global motion of interstellar matter including the effects of cosmic-ray and magnetic-field pressure is presented. First an adiabatic equation of state for the thermal background plasma and a loss-free cosmic-ray gas in the strong-scattering limit is considered. In this case only one type of flow is consistent with the physical constraints: a subsonic wind at the base which accelerates for all values of galactic height (z) but never becomes supersonic. Second, a nonadiabatic interstellar gas is discussed. Including additional heating causes an acceleration to higher velocities. The presented solutions can be used to model halo components of interstellar matter with large-scale heights.
Interstellar matter and nebulae PACS 96.40 Cosmic rays
Plasma flow magnetohydrodynamics
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D. Breitschwerdt, H. J. Völk andJ. F. McKenzie:Proceedings of the XX International Cosmic Ray Conference, Moscow, 1987, V.2, p. 115;D. Breitschwerdt, J. F. McKenzie andH. J. Völk:Proceedings of the XXI International Cosmic Ray Conference, Adelaide, 1990, V.3, p. 315.Google Scholar
J. F. McKenzie, D. Breitschwerdt andH. J. Völk:Proceedings of the XX International Cosmic Ray Conference, Moscow, 1987, V.2, p. 119.Google Scholar
M. K. Dougherty, D. Breitschwerdt andH. J. Völk:Proceedings of the XXI International Cosmic Ray Conference, Adelaide, 1990, V.3, p. 319.Google Scholar