Formation and evolution of the disc in spiral galaxies - Viscous models without infall

Details Formation and evolution of the disc in spiral galaxies - Viscous models without infall Formation and evolution of the disc in spiral galaxies - Viscous models without infall

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.252..102o&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 252, Sept. 1, 1991, p. 102-115.

Astronomy and Astrophysics

Astronomy

18

Galactic Evolution, Galactic Structure, Spiral Galaxies, Star Distribution, Star Formation, Accretion Disks, Angular Momentum, Interstellar Gas, Lyman Alpha Radiation, Quasars

Scientific paper

Models for the evolution of the disk of spiral galaxies that include the effects of viscosity but assume no continuous infall of gas on to the disk are studied. The time-scale for star formation is assumed to be of the same order as the time-scale for viscous redistribution of the mass and angular momentum in the disk. It is confirmed that these models are able to reproduce the observed radial distribution of gas and stars for present-day spirals for a variety of model parameters and initial conditions. Furthermore, it is generally found that the evolution of both the stellar and gas surface density profiles is approximately self-similar over at least 90 percent of the history of the disk, and that the size of the initial gas disk is approximately equal to the present Holmberg radius for the galaxy. Implications of these results for the evolution of spiral structure and for the interpretation of damped Ly-alpha lines in the spectra of high-redshift QSOs are considered. A discussion of the possible physical mechanisms for the viscosity and the associated time-scales is also presented.

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