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The Chemodynamical Evolution of Spheroidal Systems and the Resultant Stellar Abundance Distribution Function

Published online by Cambridge University Press:  25 May 2016

T. Tsujimoto ,
T. Shigeyama  and
K. Nomoto
T. Tsujimoto
Affiliation:
National Astronomical Observatory Mitaka, Tokyo 181, Japan
T. Shigeyama
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
K. Nomoto
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan

Extract

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We construct a chemo-dynamical model for galaxy formation using a three dimensional SPH method. We simulate the formation of two spheroidal systems, i.e., the elliptical galaxy and the Galactic bulge, based on the collapse scenario for protogalaxies. We obtain the chemodynamical formation and evolution models for the two systems during the first ∼ 1 Gyr. The relative ratio of kinetic to thermal energy of supernovae is found to heavily determine the outcome. By giving the explosion energy of supernovae to the interstellar gas with a physically meaningful relative ratio of kinetic to thermal energy, the elliptical galaxy model has the hot halo and the galactic wind, but it is not the case for the Galactic bulge model.

Type
Chapter 5: How Did the Milky Way Form?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 425 - 426
Copyright
Copyright © Kluwer 1996 

References

McWilliam, A. & Rich, R.M., 1994, ApJS 91, 749 Google Scholar
Rich, R.M., 1988, AJ 362, 606 Google Scholar
Tsujimoto, T., 1994, submitted to ApJ Google Scholar