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Early disc accretion as the origin of abundance anomalies in globular clusters

Bastian, N. and Lamers, H. J. G. L. M. and de Mink, S. E. and Longmore, S. N. and Goodwin, S. P. and Gieles, M. (2013) Early disc accretion as the origin of abundance anomalies in globular clusters. Monthly Notices of the Royal Astronomical Society, 436 (3). pp. 2398-2411. ISSN 0035-8711. doi:10.1093/mnras/stt1745.

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Globular clusters (GCs), once thought to be well approximated as simple stellar populations (i.e. all stars having the same age and chemical abundance), are now known to host a variety of anomalies, such as multiple discrete (or spreads in) populations in colour–magnitude diagrams and abundance variations in light elements (e.g. Na, O, Al). Multiple models have been put forward to explain the observed anomalies, although all have serious shortcomings (e.g. requiring a non-standard initial mass function of stars and GCs to have been initially 10–100 times more massive than observed today). These models also do not agree with observations of massive stellar clusters forming today, which do not display significant age spreads nor have gas/dust within the cluster. Here we present a model for the formation of GCs, where low-mass pre-main-sequence stars accrete enriched material released from interacting massive binary and rapidly rotating stars on to their circumstellar discs, and ultimately on to the young stars. As was shown in previous studies, the accreted material matches the unusual abundances and patterns observed in GCs. The proposed model does not require multiple generations of star formation, conforms to the known properties of massive clusters forming today and solves the ‘mass budget problem’ without requiring GCs to have been significantly more massive at birth. Potential caveats to the model as well as model predictions are discussed.

Item Type:Article
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URLURL TypeDescription Paper DOIArticle
de Mink, S. E.0000-0001-9336-2825
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 September 12. Received 2013 September 12; in original form 2013 August 10. First published online: October 9, 2013. We thank Nathan Mayne, Jay Strader, Diederik Kruijssen, Nick Moeckel and Phil Armitage for insightful discussions. NB and MG are partially funded by University Research Fellowships from the Royal Society. SdM acknowledges support by NASA through Hubble Fellowship grant HST-HF-51270.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555 and the Einstein Fellowship programme through grant PF3-140105 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under the contract NAS8-03060. We also thank the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the conception and writing of this paper.
Funding AgencyGrant Number
Royal Society University Research FellowshipUNSPECIFIED
NASA Hubble FellowshipHST-HF-51270.01-A
NASA Einstein FellowshipPF3-140105
Subject Keywords:globular clusters: general; galaxies: star clusters: general
Issue or Number:3
Record Number:CaltechAUTHORS:20140131-073421636
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43597
Deposited By: Tony Diaz
Deposited On:02 Mar 2014 14:54
Last Modified:10 Nov 2021 16:40

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