Helium core white dwarfs in globular clusters

Brad M.S. Hansen*, Vicky Kalogera, Frederic A Rasio

*Corresponding author for this work

Research output: Contribution to journalReview article

21 Citations (Scopus)

Abstract

We examine the theoretical implications of a population of low-mass helium core white dwarfs in globular clusters. In particular, we focus on the observed population in the core of NGC 6397, where several low-mass white dwarf candidates have been identified as "nonflickerers" by Cool and collaborators. Age and mass estimates from cooling models, combined with dynamical and evolutionary considerations, lead us to infer that the dark binary companions are C/O white dwarfs rather than neutron stars. Furthermore, we find that the progenitor binaries very likely underwent an exchange interaction within the last 109 yr. We examine the prospects for detecting a similar population in other globular clusters, with particular attention to the case of 47 Tuc.

Original languageEnglish (US)
Pages (from-to)1364-1373
Number of pages10
JournalAstrophysical Journal
Volume586
Issue number2 I
DOIs
StatePublished - Apr 1 2003

Fingerprint

globular clusters
helium
neutron stars
cooling
estimates
interactions

Keywords

  • Binaries: close
  • Globular clusters: general
  • Globular clusters: individual (NGC 6397, 47 Tucanae)
  • Hertzsprung-Russell diagram
  • Stellar dynamics
  • White dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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title = "Helium core white dwarfs in globular clusters",
abstract = "We examine the theoretical implications of a population of low-mass helium core white dwarfs in globular clusters. In particular, we focus on the observed population in the core of NGC 6397, where several low-mass white dwarf candidates have been identified as {"}nonflickerers{"} by Cool and collaborators. Age and mass estimates from cooling models, combined with dynamical and evolutionary considerations, lead us to infer that the dark binary companions are C/O white dwarfs rather than neutron stars. Furthermore, we find that the progenitor binaries very likely underwent an exchange interaction within the last 109 yr. We examine the prospects for detecting a similar population in other globular clusters, with particular attention to the case of 47 Tuc.",
keywords = "Binaries: close, Globular clusters: general, Globular clusters: individual (NGC 6397, 47 Tucanae), Hertzsprung-Russell diagram, Stellar dynamics, White dwarfs",
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}

Helium core white dwarfs in globular clusters. / Hansen, Brad M.S.; Kalogera, Vicky; Rasio, Frederic A.

In: Astrophysical Journal, Vol. 586, No. 2 I, 01.04.2003, p. 1364-1373.

Research output: Contribution to journalReview article

TY - JOUR

T1 - Helium core white dwarfs in globular clusters

AU - Hansen, Brad M.S.

AU - Kalogera, Vicky

AU - Rasio, Frederic A

PY - 2003/4/1

Y1 - 2003/4/1

N2 - We examine the theoretical implications of a population of low-mass helium core white dwarfs in globular clusters. In particular, we focus on the observed population in the core of NGC 6397, where several low-mass white dwarf candidates have been identified as "nonflickerers" by Cool and collaborators. Age and mass estimates from cooling models, combined with dynamical and evolutionary considerations, lead us to infer that the dark binary companions are C/O white dwarfs rather than neutron stars. Furthermore, we find that the progenitor binaries very likely underwent an exchange interaction within the last 109 yr. We examine the prospects for detecting a similar population in other globular clusters, with particular attention to the case of 47 Tuc.

AB - We examine the theoretical implications of a population of low-mass helium core white dwarfs in globular clusters. In particular, we focus on the observed population in the core of NGC 6397, where several low-mass white dwarf candidates have been identified as "nonflickerers" by Cool and collaborators. Age and mass estimates from cooling models, combined with dynamical and evolutionary considerations, lead us to infer that the dark binary companions are C/O white dwarfs rather than neutron stars. Furthermore, we find that the progenitor binaries very likely underwent an exchange interaction within the last 109 yr. We examine the prospects for detecting a similar population in other globular clusters, with particular attention to the case of 47 Tuc.

KW - Binaries: close

KW - Globular clusters: general

KW - Globular clusters: individual (NGC 6397, 47 Tucanae)

KW - Hertzsprung-Russell diagram

KW - Stellar dynamics

KW - White dwarfs

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