Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-23T13:52:37.434Z Has data issue: false hasContentIssue false
  • English
  • Français

SPH Simulations of the Chemical and Dynamical Evolution of the Galactic Bulge

Published online by Cambridge University Press:  07 August 2017

T. Tsujimoto ,
K. Nomoto ,
T. Shigeyama  and
Y. Ishimaru
T. Tsujimoto
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
K. Nomoto
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
T. Shigeyama
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
Y. Ishimaru
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We simulate the chemical and dynamical evolution of the galactic bulge with the smoothed particle hydrodynamics (SPH) method. We calculate the early phase of galaxy formation in which the bulge is formed through a burst of star formation. The calculated abundance distribution function of stars in the bulge is consistent with the observations of bulge K giants, if the heavy element yields are three times larger than those expected from Salpeter's IMF.

Keywords

galaxies: dynamicsabundancessupernovae
Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 395 - 396
Copyright
Copyright © Kluwer 1993 

References

Matteucci, F., Brocato, E., 1990, ApJ, 365, 539.Google Scholar
Rich, R.M., 1990, ApJ, 362, 606.Google Scholar
Rich, R.M., 1992, in IAU Symposium 149, The Stellar Populations of Galaxies (Kluwer), p. 29.Google Scholar