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Galaxies 2017, 5(3), 36; doi:10.3390/galaxies5030036

How Clumpy Star Formation Affects Globular Cluster Systems

Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA
Academic Editors: Duncan A. Forbes and Ericson D. Lopez
Received: 7 June 2017 / Revised: 31 July 2017 / Accepted: 2 August 2017 / Published: 4 August 2017
(This article belongs to the Special Issue On the Origin (and Evolution) of Baryonic Galaxy Halos)
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Abstract

There is now clear evidence the metallicities of globular clusters are not simple tracers of the elemental abundances in their protocluster clouds; some of the heavy elements were formed subsequently within the cluster itself. It is also manifestly clear that star formation is a clumpy process. We present a brief overview of a theoretical model for how self-enrichment by supernova ejecta proceeds in a protocluster undergoing clumpy star formation, and show that it predicts internal abundance spreads in surprisingly good agreement with those in observed Milky Way clusters. View Full-Text
Keywords: globular clusters; star formation; abundances; stellar halos globular clusters; star formation; abundances; stellar halos
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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).

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Bailin, J. How Clumpy Star Formation Affects Globular Cluster Systems. Galaxies 2017, 5, 36.

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