Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...199..114m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 199, no. 1-2, June 1988, p. 114-126.
Astronomy and Astrophysics
Astrophysics
14
Astronomical Models, Galactic Evolution, Gas Dynamics, Hydrodynamic Equations, Interstellar Gas, Temperature Distribution, Collisions, Flow Distribution, Luminosity
Scientific paper
The dynamical and thermal evolution of the warm component of the interstellar medium during a fast head-on collision of two galaxies is investigated by means of two-dimensional hydrodynamic simulations. The dynamics of the stellar component of the galaxies is not followed in detail, but its influence on the gas is incorporated into the model through its gravitational potential, which is assumed to be of fixed shape. The collision of the galaxies is simulated by a constant relative motion of the two potential wells, which contain the isothermal interstellar gas in hydrostatic equilibrium. Radiative losses of the gas are calculated with the aid of a cooling function, and the self-gravity of the gas component is neglected. In the given parameter space (relative velocity, escape velocity, and chemical composition of the interstellar matter) the total gas content of the collidng galaxies is swept out. In the case of a large relative velocity (2000 km/s) the matter is leaving the galaxies in form of hot gas, while for a smaller relative velocity (1000 km/s) the gas forms a cool, disklike, probably gravitationally bound object between the withdrawing galaxies.
Arnold C. N.
Hillebrandt Wolfgang
Mair G.
Mueller Ewald
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