Dissipation, merging and the rotation of galaxies

Details Dissipation, merging and the rotation of galaxies Dissipation, merging and the rotation of galaxies

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.281..200f&link_type=abstract

Nature, vol. 281, Sept. 20, 1979, p. 200-202.

Computer Science

41

Disk Galaxies, Elliptical Galaxies, Galactic Evolution, Galactic Rotation, Galactic Clusters, Gravitational Effects, Spin Dynamics, Stellar Models, Velocity Distribution

Scientific paper

A model for the formation of disk galaxies by dissipation and bright elliptical galaxies by galactic merging is presented, with attention given to the galactic rotation properties predicted. The proposed evolutionary sequence consists of pregalactic haloes formed by the gravitational clustering of low-mass or burnt-out stars and residual gas, which cool and collapse into disk galaxies with a characteristic spin derived from the tidal spin of the halo and the conservation of angular momentum. The hierarchical clustering and merging of the disk galaxies in small groups then leads to the formation of elliptical galaxies, with spins derived primarily from the orbital angular momentum of the disk galaxies preceeding them. Calculations of the spin parameters predicted by the model are shown to be in reasonable agreement with observations, indicating the compatibility of the model with the formation of at least some bright elliptical galaxies.

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