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Galaxy Morphology in Dissipative Models

Published online by Cambridge University Press:  03 August 2017

M. B. Mosconi  and
D. Garcia Lambas
M. B. Mosconi
Affiliation:
Observatorio Astronómico Laprida 854 5000 - Córdoba Argentina
D. Garcia Lambas
Affiliation:
Observatorio Astronómico Laprida 854 5000 - Córdoba Argentina

Abstract

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Using numerical simulations in the context of a simple dissipative model (Abadi et al. 1990) we study the final morphologies and dynamical properties of galaxies under different initial conditions. The protogalaxies are embedded in dynamically relaxed potential wells of dark matter with different initial spin parameters λ and velocity dispersions σ in the dissipative component. We find that both λ and σ control the final morphology of the galaxies. The angular momentum might be acquired by tidal torques, and several sources may account for the velocity dispersion. For instance, under the assumption that supernovae explosions provide kinetic energy to the medium giving σ ∼ 8-10 km/s (Mc Kee & Ostriker 1977) our models suggest that the border line spin parameter between early type and late type morphologies would be approximately λ ∼ 0.04.

Type
XI- Galaxy Evolution
Information
Symposium - International Astronomical Union , Volume 146: Dynamics of Galaxies and their Molecular Cloud Distributions , 1991 , pp. 379 - 382
Copyright
Copyright © Kluwer 1991 

References

Abadi, M., García Lambas, D. and Mosconi, M. B. 1990, Ap. J. 359, in press.Google Scholar
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Hoffman, Y. 1988, Ap. J., 329, 8.Google Scholar
Mc Kee, C. and Ostriker, J. 1977, Ap. J. 233, 148.Google Scholar
Tissera, P. and Lambas, D.G. 1990, MNRAS, in press.Google Scholar