Rotation of halos in open and closed universes - Differentiated merging and natural selection of galaxy types

Details Rotation of halos in open and closed universes - Differentiated merging and natural selection of galaxy types Rotation of halos in open and closed universes - Differentiated merging and natural selection of galaxy types

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...330..519z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 330, July 15, 1988, p. 519-534.

Astronomy and Astrophysics

Astrophysics

127

Cosmology, Dark Matter, Galactic Structure, Angular Momentum, Baryons, Computerized Simulation, Density (Mass/Volume), Elliptical Galaxies, Galactic Evolution, Halos, Spiral Galaxies

Scientific paper

Computer simulations are used here to study the properties of galactic halos formed from Gaussian initial density perturbations in both open and closed dark matter universes. It is shown that if galaxies form through gravitational collapse from initial, Gaussian density perturbations, then their luminous parts do not have the 'original' values of either specific angular momentum (ellipticals) or spin parameter lambda (spirals). The rotational properties of a halo depend only weakly on either the halo density or the density of its environment. Variations of the large-scale density of the environment have an expected, dramatic effect on the density of individual halos. Dissipationless merging forces the cores of the merging objects into the core of the merger product. In the process, cores become more bound and lose angular momentum. These findings are extrapolated to propose a model for galaxy formation in which both ellipticals and spirals come into being through mergers.

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