Simulations of the effect of spiral arms on the cloud-ensemble velocity dispersion

Details Simulations of the effect of spiral arms on the cloud-ensemble velocity dispersion Simulations of the effect of spiral arms on the cloud-ensemble velocity dispersion

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...250..316t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 2, Oct. 1991, p. 316-323.

Astronomy and Astrophysics

Astrophysics

19

Interstellar Matter, Many Body Problem, Molecular Clouds, Spiral Galaxies, Computerized Simulation, Velocity Distribution

Scientific paper

N-body simulations are used to study the effect of spiral heating, viscous heating, and cooling by inelastic collisions on the molecular cloud ensemble velocity dispersion. The simulations include inelastic collisions between clouds as well as long-range gravitational forces. The theory for heating and cooling of the cloud population is described, and the numerical code and the galaxy model are examined. Spiral arms not only heat the cloud population, they also cause increased cooling due to the large number of cloud-cloud collisions in the arms. It is found that the heating dominates, in that a stronger spiral potential leads to a higher velocity dispersion. The spiral potential is stronger for smaller values of Q(star). The steady-state cloud-ensemble velocity dispersion is found to be constant with the radius. Its value for a typical simulation of a multiple-arm spiral is slightly smaller than the value observed in the Galaxy. The stellar velocity dispersion corresponds to a radius-independent Q(star), for multiple-arm galaxies regardless of the initial radial dependence.

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