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Issue A&A
Volume 436, Number 1, June II 2005
Page(s) 145 - 154
Section Galactic structure, stellar clusters and populations
DOI http://dx.doi.org/10.1051/0004-6361:20042275



A&A 436, 145-154 (2005)
DOI: 10.1051/0004-6361:20042275

Self-enrichment in globular clusters

I. An analytic approach
S. Recchi1, 2, 3 and I. J. Danziger3

1  University Observatory of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
    e-mail: recchi@astro.univie.ac.at
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: danziger@ts.astro.it

(Received 28 October 2004 / Accepted 21 February 2005)

Abstract
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 $M_\odot$. 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

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