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Type Ia Supernovae and Planets in Star Clusters

Published online by Cambridge University Press:  26 May 2016

Michael M. Shara  and
Jarrod R. Hurley
Michael M. Shara
Affiliation:
Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024
Jarrod R. Hurley
Affiliation:
Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024

Abstract

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Star clusters are remarkably efficient (relative to the field) at making type Ia supernovae candidates: very short period, massive double-white-dwarf stars and giant-white dwarf binaries. The high frequency of these systems is the result of dynamical encounters between (mostly) primordial binaries and other cluster stars. Orbital hardening rapidly drives the degenerate binaries to periods under ∼ 10 hours. Gravitational radiation emission and mergers then produce supra-Chandrasekhar objects in less than a Hubble time.

We also find that free-floating planets can remain bound to a star cluster for much longer than was previously assumed: of the order of the cluster half-mass relaxation timescale as opposed to the crossing-time. The planets in our N-body study are of Jupiter mass and are initially placed in circular orbits of between 0.05 and 50 AU about a parent star whose mass is chosen from a realistic initial mass function. This result is important in the context of the preliminary detection of a population of free-floating sub-stellar objects in the globular cluster M22.

Type
Planetary Formation
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 53 - 60
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Aarseth, S. J. 1999, PASP, 111, 1333 Google Scholar
Bonnell, I. A., Smith, K. W., Davies, M. B., & Home, K. 2001, MNRAS, 322, 859 Google Scholar
Gilliland, R. L., et al. 2000, ApJ, 545, L47 Google Scholar
Hurley, J.R., Pols, O.R., & Tout, C.A. 2000, MNRAS, 315, 543 Google Scholar
Hurley, J. R., Tout, C. A., Aarseth, S. J., & Pols, O.R. 2001, MNRAS, 323, 630 Google Scholar
Hurley, J.R., Tout, C.A., & Pols, O.R. 2002, MNRAS, accepted Google Scholar
Kroupa, P., Tout, C. A., & Gilmore, G. 1993, MNRAS, 262, 545 Google Scholar
Makino, J. 2002, in ASP Conf. Ser. XX, Stellar Collisions, Mergers and their Consequences, ed. Shara, M. M. (San Francisco: ASP), in press Google Scholar
Perlmutter, S., et al. 1999, ApJ, 517, 565 CrossRefGoogle Scholar
Phillips, M.M., 1993, ApJ, 413L, 105 Google Scholar
Riess, A.G. et al. 1998, AJ, 116, 1009 Google Scholar
Riess, A.G. 2000, PASP, 112, 1284 Google Scholar
Sahu, K. C., Casertano, S., Livio, M., Gilliland, R. L., Panagia, N., Albrow, M. D., & Potter, M. 2001, Nature, 411, 1022 Google Scholar
Smith, K. W., & Bonnell, I. A. 2001, MNRAS, 322, L1 CrossRefGoogle Scholar
Yungelson, L., Livio, M., ApJ, 528, 108 Google Scholar