Dissipative models of spiral galaxies

Abstract

view Abstract Citations (97) References (13) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Dissipative models of spiral galaxies Carlberg, R. G. ; Freedman, W. L. Abstract Self-consistent N-body experiments have been performed for a galactic disk containing both stars and a dissipative gas component. The gas is treated with a simple sticky particle scheme, which maintains the gas at a low velocity dispersion and results in continuous dynamical cooling of the disk. The disks exhibit dramatic activity, with both the stars and the gas showing large-scale spiral structure. The gas arms generally overlie the stellar arms but are much narrower and show structure on smaller scales than the stars. The number of spiral arms m is found to be strongly correlated with the fraction of the total mass in the disk f, such that m is approximately equal to 1/f as expected from swing amplification theory. A population of disk stars with a large velocity dispersion (Q of about 2.5) is shown to be so 'stiff' that it is effectively in the halo, as far as spiral activity is concerned. The gas loses angular momentum to the stars, resulting in a slow inward radial flow on a time scale of about 100 revolutions. Publication: The Astrophysical Journal Pub Date: November 1985 DOI: 10.1086/163634 Bibcode: 1985ApJ...298..486C Keywords: Astronomical Models; Galactic Structure; Spiral Galaxies; Star Distribution; Angular Momentum; Galactic Evolution; Many Body Problem; Astrophysics full text sources ADS |