The Formation of the Hubble Sequence of Disk Galaxies: the Effects of Early Viscous Evolution

Details The Formation of the Hubble Sequence of Disk Galaxies: the Effects of Early Viscous Evolution The Formation of the Hubble Sequence of Disk Galaxies: the Effects of Early Viscous Evolution

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19513605z&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #136.05; Bulletin of the American Astronomical Society, Vol. 32, p.884

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a model of disk galaxies whereby viscous evolution of the gaseous disk drives material inwards to form a proto-bulge. We first derive generic analytic solutions for the disk-halo system under the standard disk formation scenario, and give limits on the final density profile of the dark halo in the central regions, after adiabatic compression. With some appropriate assumptions, we can mimic the viscous evolution of disk, coupled with star formation, with analytic variation of the specific angular momentum distribution of the disk. We find that the present properties of disks, such as the scale length, are compatible with a higher initial formation redshift if the re-distribution by viscous evolution is included than if it is ignored. Focusing on small `exponential' bulges, ones that may be formed through a disk instability, we investigate the relationship between the assumed initial conditions, such as halo `formation', or assembly, redshift zf, spin parameter λ , baryonic fraction F, and final disk properties such as global star formation timescale, gas fraction, and bulge-to-disk ratio. We acknowledge support from NASA, ATP Grant NAG5-3928.

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