On the thermal structure and stability of configurations with heat diffusion and a gain-loss function. II - Application to the interstellar medium

Details On the thermal structure and stability of configurations with heat diffusion and a gain-loss function. II - Application to the interstellar medium On the thermal structure and stability of configurations with heat diffusion and a gain-loss function. II - Application to the interstellar medium

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..625p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 2, p. 625-633.

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Applications

6

Interstellar Matter, Magnetohydrodynamic Stability, Plasma Diffusion, Thermal Conductivity, High Temperature Gases, Plasma Oscillations, Thermal Plasmas

Scientific paper

The thermal structure and stability of steady configurations are determined assuming that they are constituted of a gas heated at a rate about T exp m, cooled at a rate about T exp n, and with a thermal conductivity coefficient T exp k. General results are obtained for a plasma with solar abundances in the range of temperature between 10 exp 2 and 10 exp 8 K, where the cooling function is parameterized by means of ten different values of the exponent n. Applications to different regions of the interstellar medium are emphasized. In particular, when the plasma is thermally unstable, the radius, mass, and growing time of the fastest growing mode are calculated as functions of the equilibrium pressure and temperature. The results suggest that the Galactic halo gas could be close to a marginal state. Henceforth, a thermal instability could work as a feed-back mechanism of mass exchange between the halo and the Galactic disk. Additionally, the thermal characteristics of the most probable structure that can be formed and the threshold amplitude beyond which nonlinear instability develops are also obtained.

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