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The Formation of Disks in Galaxies

Published online by Cambridge University Press:  07 August 2017

G. Hensler ,
A. Burkert ,
J. W. Truran ,
H. Dünhuber  and
C. Theis
G. Hensler
Affiliation:
Inst. of Theoretical Physics and Observatory, University of Kiel, Olshausenstr. 40, D-2300 Kiel 1, Fed. Rep. of Germany
A. Burkert
Affiliation:
Dept. of Astronomy, University of Illinois, 1011 West Springfield Ave., Urbana Champaign, IL 61801, USA University of California, Lick Observatory, Santa Cruz, CA 95064, USA
J. W. Truran
Affiliation:
Dept. of Astronomy, University of Illinois, 1011 West Springfield Ave., Urbana Champaign, IL 61801, USA
H. Dünhuber
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-8046 Garching, Fed. Rep. of Germany
C. Theis
Affiliation:
Inst. of Theoretical Physics and Observatory, University of Kiel, Olshausenstr. 40, D-2300 Kiel 1, Fed. Rep. of Germany

Abstract

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Different chemo-dynamical models dealing with the formation of stellar disks in the course of galaxy evolution are presented. One-dimensional models concerning the vertical stratification of disks are in strikingly good agreement with the solar vicinity. Two-dimensional investigations of the global evolution of disk galaxies show from preliminary results that the disk formation is delayed by means of an equatorial outflow of hot metal-enriched gas that stems from supernova ejecta in the star-forming central region.

Type
I. The Stellar Populations in the Milky Way
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 119 - 122
Copyright
Copyright © Kluwer