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The Formation of the Galactic Bulge

Published online by Cambridge University Press:  25 May 2016

M. Samland  and
G. Hensler
M. Samland
Affiliation:
Institut für Astronomie und Astrophysik, Universität Kiel, D-24098 Kiel, Germany
G. Hensler
Affiliation:
Institut für Astronomie und Astrophysik, Universität Kiel, D-24098 Kiel, Germany

Extract

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The question is adressed whether the problem of the stellar metallicity distribution and the dynamics of the stellar components in the bulge as found out by refined observations during recent years can be understood within the context of the evolution of the whole Galaxy. A selfconsistent galaxy model has to explain the apparent differences in the effective yields of the enrichment of bulge, disk and halo. Moreover, it has to account for the observed age-metallicity distribution of the stellar components. It appears that chemo-dynamical infall models provide a consistent description of the bulge, in particular the metallicity distribution of the K giants. It should be emphasized that simple closed-box models are not appropriate, because during the bulge formation there is infall of cloudy medium (CM), as well as outflow of hot, ionized gas ejected by supernovae type II (SNII). Therefore dynamical processes have to be taken into account. For details of the chemo-dynamical description we refer to Samland & Hensler (1994) and references therein.

Type
Chapter 5: How Did the Milky Way Form?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 429 - 430
Copyright
Copyright © Kluwer 1996 

References

McWilliam, A., Rich, R.M., (1994), Astrophys. J. Suppl. 91,749 CrossRefGoogle Scholar
Rich, R.M., (1988), Astron. J. 95,828 CrossRefGoogle Scholar
Samland, M., Hensler, G., (1994), Metal Pre-Enrichment of the Galactic Disk in: IAU Symp. No. 169, Unsolved Problems of the Milky Way , ed. Blitz, L. Google Scholar