Bounds on expected black hole spins in inspiraling binaries

R. O'Shaughnessy*, J. Kaplan, Vicky Kalogera, K. Belczynski

*Corresponding author for this work

Research output: Contribution to journalReview article

29 Citations (Scopus)

Abstract

As a first step toward understanding the angular momentum evolution history of black holes in merging black hole/neutron star binaries, we perform population synthesis calculations to track the distribution of accretion histories of compact objects in such binaries. We find that there are three distinct processes that can possibly contribute to the black hole spin magnitude: a birth spin for the black hole, imparted at either (1) the collapse of a massive progenitor star to a black hole or (2) the accretion-induced collapse of a neutron star to a black hole, and (3) an accretion spin-up when the already formed black hole (via processes 1 or 2) goes through an accretion episode (through an accretion disk or a common-envelope phase). Our results show that, with regard to accretion-induced spin-up in merging BH-NS binaries (method 3 above), only accretion episodes associated with common-envelope phases and hypercritical accretion rates occur in the formation history of merging black hole/neutron star binaries. Lacking unambiguous experimental information about BH birth spins (i.e., regarding the results of processes 1 and 2), we choose two fiducial values for the BH birth angular momentum parameter a = J/M2, consistent with observations of (1) NS birth spins (a ≃ 0) and (2) X-ray binaries (a = 0.5). Using these two fiducial values and a conservative upper bound on the specific angular momentum of accreted matter, we discuss the expected range of black hole spins in the binaries of interest. We conclude with comments on the significance of these results for ground-based gravitational wave searches of inspiral signals from black hole binaries.

Original languageEnglish (US)
Pages (from-to)1035-1041
Number of pages7
JournalAstrophysical Journal
Volume632
Issue number2 I
DOIs
StatePublished - Oct 20 2005

Fingerprint

accretion
angular momentum
neutron stars
histories
history
envelopes
massive stars
accretion disks
gravitational waves
synthesis
x rays

Keywords

  • Binaries: close
  • Black hole physics
  • Stars: neutron
  • Stars: rotation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

O'Shaughnessy, R. ; Kaplan, J. ; Kalogera, Vicky ; Belczynski, K. / Bounds on expected black hole spins in inspiraling binaries. In: Astrophysical Journal. 2005 ; Vol. 632, No. 2 I. pp. 1035-1041.
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O'Shaughnessy, R, Kaplan, J, Kalogera, V & Belczynski, K 2005, 'Bounds on expected black hole spins in inspiraling binaries', Astrophysical Journal, vol. 632, no. 2 I, pp. 1035-1041. https://doi.org/10.1086/444346

Bounds on expected black hole spins in inspiraling binaries. / O'Shaughnessy, R.; Kaplan, J.; Kalogera, Vicky; Belczynski, K.

In: Astrophysical Journal, Vol. 632, No. 2 I, 20.10.2005, p. 1035-1041.

Research output: Contribution to journalReview article

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T1 - Bounds on expected black hole spins in inspiraling binaries

AU - O'Shaughnessy, R.

AU - Kaplan, J.

AU - Kalogera, Vicky

AU - Belczynski, K.

PY - 2005/10/20

Y1 - 2005/10/20

N2 - As a first step toward understanding the angular momentum evolution history of black holes in merging black hole/neutron star binaries, we perform population synthesis calculations to track the distribution of accretion histories of compact objects in such binaries. We find that there are three distinct processes that can possibly contribute to the black hole spin magnitude: a birth spin for the black hole, imparted at either (1) the collapse of a massive progenitor star to a black hole or (2) the accretion-induced collapse of a neutron star to a black hole, and (3) an accretion spin-up when the already formed black hole (via processes 1 or 2) goes through an accretion episode (through an accretion disk or a common-envelope phase). Our results show that, with regard to accretion-induced spin-up in merging BH-NS binaries (method 3 above), only accretion episodes associated with common-envelope phases and hypercritical accretion rates occur in the formation history of merging black hole/neutron star binaries. Lacking unambiguous experimental information about BH birth spins (i.e., regarding the results of processes 1 and 2), we choose two fiducial values for the BH birth angular momentum parameter a = J/M2, consistent with observations of (1) NS birth spins (a ≃ 0) and (2) X-ray binaries (a = 0.5). Using these two fiducial values and a conservative upper bound on the specific angular momentum of accreted matter, we discuss the expected range of black hole spins in the binaries of interest. We conclude with comments on the significance of these results for ground-based gravitational wave searches of inspiral signals from black hole binaries.

AB - As a first step toward understanding the angular momentum evolution history of black holes in merging black hole/neutron star binaries, we perform population synthesis calculations to track the distribution of accretion histories of compact objects in such binaries. We find that there are three distinct processes that can possibly contribute to the black hole spin magnitude: a birth spin for the black hole, imparted at either (1) the collapse of a massive progenitor star to a black hole or (2) the accretion-induced collapse of a neutron star to a black hole, and (3) an accretion spin-up when the already formed black hole (via processes 1 or 2) goes through an accretion episode (through an accretion disk or a common-envelope phase). Our results show that, with regard to accretion-induced spin-up in merging BH-NS binaries (method 3 above), only accretion episodes associated with common-envelope phases and hypercritical accretion rates occur in the formation history of merging black hole/neutron star binaries. Lacking unambiguous experimental information about BH birth spins (i.e., regarding the results of processes 1 and 2), we choose two fiducial values for the BH birth angular momentum parameter a = J/M2, consistent with observations of (1) NS birth spins (a ≃ 0) and (2) X-ray binaries (a = 0.5). Using these two fiducial values and a conservative upper bound on the specific angular momentum of accreted matter, we discuss the expected range of black hole spins in the binaries of interest. We conclude with comments on the significance of these results for ground-based gravitational wave searches of inspiral signals from black hole binaries.

KW - Binaries: close

KW - Black hole physics

KW - Stars: neutron

KW - Stars: rotation

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U2 - 10.1086/444346

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