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The Chemical Evolution of Heavy Elements in Globular Clusters

Published online by Cambridge University Press:  06 January 2014

Luke J. Shingles ,
Amanda I. Karakas  and
Raphael Hirschi
Luke J. Shingles
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Australia
Amanda I. Karakas
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Australia
Raphael Hirschi
Affiliation:
Astrophysics Group, Lennard-Jones Laboratories, EPSAM, Keele University, UK Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, Japan
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Abstract

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We present preliminary results from a chemical evolution model that tracks the composition of heavy elements beyond iron in a globular cluster. The heavy elements can be used as tracers of the nucleosynthetic events that defined the formation and evolution of star clusters in the early Universe. In particular, the chemical evolution model focuses on the hypothesis that rapidly-rotating massive stars produced the heavy elements via the slow neutron-capture process and seeded the proto-cluster while the stars we see today were still forming.

We compare our model with heavy element abundances in M4 and M5, and M22. Our results are strongly dependent on the highly uncertain rate of the 17O(α,γ)21Ne reaction, which determines the strength of 16O as a neutron poison. We find that the [Pb/Ba] ratio is too low to match the empirical value, which might suggest that a contribution from AGB stars is required.

Keywords

globular clusters: generalstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S298: Setting the scene for Gaia and LAMOST , May 2013 , pp. 439 - 440
Copyright
Copyright © International Astronomical Union 2014 

References

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