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Title:
The physics of dissipational galaxy formation
Authors:
Binney, J.
Affiliation:
AA(Princeton University, New Observatory, Princeton, N.J.)
Publication:
Astrophysical Journal, Part 1, vol. 215, July 15, 1977, p. 483-491. Research supported by Magdalen College and Lindemann Trust. (ApJ Homepage)
Publication Date:
07/1977
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ASTRONOMICAL MODELS, ENERGY DISSIPATION, GALACTIC EVOLUTION, GRAVITATIONAL COLLAPSE, HYDRODYNAMICS, ELLIPTICAL GALAXIES, GALACTIC STRUCTURE, GAS MIXTURES, HELIUM, HYDROGEN CLOUDS, SHOCK FRONTS
Comment:
A&AA ID. AAA019.158.142
DOI:
10.1086/155378
Bibliographic Code:
1977ApJ...215..483B

Abstract

The literature on nonlinear stages of galaxy formation is briefly reviewed along with arguments that lead to the consideration of a dissipative formation process. Hydrodynamic calculations are presented for the collapse of protogalactic gas clouds at redshifts less than 10; it is assumed that the clouds do not fragment during their first infall, so that the collapse is halted by shock-front formation about a caustic surface. The cooling, later fragmentation, evaporation, and binding-energy loss of such clouds are investigated, and ways in which these processes may have influenced the formation of elliptical and disk galaxies are discussed. A simple model for the formation of the Hubble sequence is outlined in which mass and perturbation morphology, together with the physics governing the cooling of a hydrogen-helium mixture, determine the type of galaxy that is formed from a whole range of protogalactic clouds.

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