Large-scale flow of interstellar gas in galactic spiral waves - Effects of thermal balance and self-gravitation

Details Large-scale flow of interstellar gas in galactic spiral waves - Effects of thermal balance and self-gravitation Large-scale flow of interstellar gas in galactic spiral waves - Effects of thermal balance and self-gravitation

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..89..177m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 89, no. 1, Jan. 1983, p. 177-199.

Other

14

Galactic Structure, Gas Flow, Hydrogen Clouds, Interstellar Gas, Milky Way Galaxy, Spiral Galaxies, Astronomical Models, Cooling, Density Wave Model, Gravitational Fields, Heating, Isothermal Flow, Shock Waves

Scientific paper

Recent observational data on atomic and molecular hydrogen in the Galaxy are used to analyze the dynamics of the interstellar gas in a spiral density wave. Following the model of the galactic spiral structure proposed by Marochnik et al. (1972), the gas flow is obtained, with an allowance made for self-gravitation and thermal processes. There are three principal findings. The first is that the self-gravitation of gas does not significantly affect the galactic shock if the dominant contribution to the gas density comes from atomic hydrogen. The second is that the effects of self-gravitation could be essential for both the gas flow and the stellar spiral wave only if the density contribution of H2 is several times that of H I (with molecular hydrogen as a continuous medium having the isothermal equation of state). The third finding is that regardless of the estimates of H2 abundance in the Galaxy, its reaction to the density wave is weak since it forms a collisionless system not dragged by the intercloud gas.

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