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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
Galaxies 2017, 5(3), 36;
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)
PDF [717 KB, uploaded 5 August 2017]


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

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