Volume 436, Number 1, June II 2005
|Page(s)||145 - 154|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||20 May 2005|
Self-enrichment in globular clusters
I. An analytic approach
University Observatory of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria e-mail: firstname.lastname@example.org
2 Institut für Theoretische Physik und Astrophysik, Kiel University, Olshausenstrasse 40, 24098 Kiel, Germany
3 INAF, Osservatorio Astronomico di Trieste, via G.B. Tiepolo, 11, 34131 Trieste, Italy e-mail: email@example.com
Accepted: 21 February 2005
By means of analytical calculations, we explore the self-enrichment scenario for Globular Cluster formation. According to this scenario, an initial burst of star formation occurs inside the core radius of the initial gaseous distribution. The outward-propagating shock wave sweeps up a shell in which gravitational instabilities may arise, leading to the formation of a second, metal-enriched, population of stars. We find a minimum mass of the proto-globular cluster of the order of 106 . We also find that the observed spread in the magnitude–metallicity relation can be explained assuming cluster-to-cluster variations of some parameters like the thermalization efficiency, the mixing efficiency and the Initial Mass Function, as well as variations of the external pressure.
Key words: Galaxy: evolution / globular clusters: general / hydrodynamics
© ESO, 2005
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