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Formation of Galaxy Disks

Published online by Cambridge University Press:  03 August 2017

Simon D.M. White
Simon D.M. White*
Affiliation:
Steward Observatory University of Arizona Tucson, AZ 85721 U.S.A.

Abstract

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Galaxy disks are observed to be young, dynamically cold, and centrifugally supported. These properties suggest that they formed in a quiescent dynamical context, reached their current configuration while still gaseous, and have been relatively undisturbed since formation. This situation can be understood if disks grow by the cooling of a gaseous atmosphere within a quasi-equilibrium dark halo. A simple version of this model can be combined with results from numerical simulations of halo formation to provide quantitative explanations for the Tully-Fisher relation, for the typical sizes of disks, and for their star formation history. A viable model seems to require stellar winds and supernovae to heat the gaseous halos of spirals via a galactic fountain. Such models predict observable X-ray halos, and suggest that continued infall replenishes the gas consumed by star formation in late-type galaxies.

Type
XI- Galaxy Evolution
Information
Symposium - International Astronomical Union , Volume 146: Dynamics of Galaxies and their Molecular Cloud Distributions , 1991 , pp. 383 - 391
Copyright
Copyright © Kluwer 1991 

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