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Grape-SPH Simulations of the Chemodynamical Evolution of Dwarf Galaxies

Published online by Cambridge University Press:  25 May 2016

Masao Mori ,
Yuzuru Yoshii ,
Takuji Tsujimoto  and
Ken'ichi Nomoto
Masao Mori
Affiliation:
Department of Astronomy, University of Tokyo, Japan
Yuzuru Yoshii
Affiliation:
Institute of Astronomy, University of Tokyo, Japan Research Center for the Early Universe, The University of Tokyo
Takuji Tsujimoto
Affiliation:
National Astronomical Observatory, Japan
Ken'ichi Nomoto
Affiliation:
Department of Astronomy, University of Tokyo, Japan Research Center for the Early Universe, The University of Tokyo

Extract

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The central concentration of the luminosity distribution in dwarf elliptical galaxies (dEs) is weaker than that of giant elliptical galaxies (Es). In other words, the luminosity profiles in Es follow the de Vaucouleurs' law whereas dEs have exponential luminosity profiles. Athanassoula(1994) describes the one dimensional simulations of the formation of dEs that include the feedback effects from supernovae. The model with no dark matter halo is shown to be much better agreements with the observations than with dark matter halo. However no attempt has yet been made to reproduce much lower heavy element abundances in dEs than in Es. We calculate the chemodynamical evolution of a less massive gas cloud with an SPH+N-body three dimensional simulation code to explore the luminosity profile and chemical abundances in dEs.

Type
Galactic Connection and Environmental Effects
Information
Symposium - International Astronomical Union , Volume 174: Dynamical Evolution of Stars Clusters , 1996 , pp. 395 - 396
Copyright
Copyright © Kluwer 1996 

References

Deckel, A. and Silk, J. (1986) ApJ 303, 39.CrossRefGoogle Scholar
Athanassoula, E. (1994) in ESO/OHP Workshop on Dwarf Galaxies., Meylan, G. & Prugniel, P., eds., ESO, Garching, p. 525.Google Scholar