Binary Mergers and Growth of Black Holes in Dense Star Clusters

O’Leary, Ryan M.; Rasio, Frederic A.; Fregeau, John M.; Іванова, Наталя; O’Shaughnessy, R.

doi:10.1086/498446

Cited by 306 publications

(332 citation statements)

References 60 publications

Supporting

Mentioning

303

Contrasting

Order By: Relevance

“…Another model [26] studies the progressive accumulation of mass into a large (> 50 M ) seed black hole via coalescence of a population of smaller black holes. However, the existence of binaries with IMBH components remains uncertain since stellar winds may stall the growth of the IMBH progenitors in the runaway collision scenario [27], or the merger recoil may also eject a newly formed black hole from the globular cluster [28,29].…”

Section: A Intermediate Mass Black Hole Formationmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

View full text Add to dashboard Cite

We present the results of a weakly modeled burst search for gravitational waves from mergers of non-spinning intermediate mass black holes (IMBH) in the total mass range 100-450 M and with the component mass ratios between 1:1 and 4:1. The search was conducted on data collected by the LIGO and Virgo detectors between November of 2005 and October of 2007. No plausible signals were observed by the search which constrains the astrophysical rates of the IMBH mergers as a function of the component masses. In the most efficiently detected bin centered on 88 + 88 M , for non-spinning sources, the rate density upper limit is 0.13 per Mpc 3 per Myr at the 90% confidence level.

show abstract

Section: A Intermediate Mass Black Hole Formationmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…However, Advanced LIGO can only detect mergers that occurred at distances P1 Gpc, i.e., relatively recently, so the relevant rate is the rate late in the history of the globular cluster, which is likely to be much lower. For example, O'Leary et al (2006) found in their numerical simulations that the rate dropped from $10 À7 to $3 ; 10 À10 yr À1 after 10 10 yr for some plausible cluster models.…”

Section: Imri Rate Per Globular Cluster and Event Ratementioning

confidence: 99%

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

Mandel

Brown

Gair

et al. 2008

ApJ

128

179

View full text Add to dashboard Cite

Gravitational waves (GWs) from the inspiral of a neutron star ( NS) or stellar-mass black hole ( BH ) into an intermediate-mass black hole ( IMBH ) with mass M $ 50 350 M may be detectable by the planned advanced generation of ground-based GW interferometers. Such intermediate mass ratio inspirals (IMRIs) are most likely to be found in globular clusters. We analyze four possible IMRI formation mechanisms: (1) hardening of an NS-IMBH or BH-IMBH binary via three-body interactions, (2) hardening via Kozai resonance in a hierarchical triple system, (3) direct capture, and (4) inspiral of a CO from a tidally captured main-sequence star; we also discuss tidal effects when the inspiraling object is an NS. For each mechanism we predict the typical eccentricities of the resulting IMRIs. We find that IMRIs will have largely circularized by the time they enter the sensitivity band of ground-based detectors. Hardening of a binary via three-body interactions, which is likely to be the dominant mechanism for IMRI formation, yields eccentricities under 10 À4 when the GW frequency reaches 10 Hz. Even among IMRIs formed via direct captures, which can have the highest eccentricities, around 90% will circularize to eccentricities under 0.1 before the GW frequency reaches 10 Hz. We estimate the rate of IMRI coalescences in globular clusters and the sensitivity of a network of three Advanced LIGO detectors to the resulting GWs. We show that this detector network may see up to tens of IMRIs per year, although rates of one to a few per year may be more plausible. We also estimate the loss in signal-to-noise ratio that will result from using circular IMRI templates for data analysis and find that, for the eccentricities we expect, this loss is negligible.

show abstract

“…Although the predicted formation rate of merging double NSs has a strong density dependence (Ivanova et al 2007), even for dense clusters like 47 Tuc the NS contribution to total cluster merger rates should be overwhelmed by double BH mergers. Such systems are expected to be formed via dynamical interactions in cluster cores (Gultekin et al 2004;O'Leary et al 2006O'Leary et al , 2008. O'Leary et al (2006O'Leary et al ( , 2008 used realistic initial conditions for their cluster simulations (which included the stellar evolution of massive stars and binaries in the first few Myr of the cluster life) and assumed immediate creation of a BH subcluster.…”

Section: Introductionmentioning

confidence: 99%

“…Such systems are expected to be formed via dynamical interactions in cluster cores (Gultekin et al 2004;O'Leary et al 2006O'Leary et al , 2008. O'Leary et al (2006O'Leary et al ( , 2008 used realistic initial conditions for their cluster simulations (which included the stellar evolution of massive stars and binaries in the first few Myr of the cluster life) and assumed immediate creation of a BH subcluster. Their calculations did not consider further stellar or binary evolution and neglected the effects of lower mass stars on BH populations.…”

Section: Introductionmentioning

confidence: 99%

The Total Merger Rate of Compact Object Binaries in the Local Universe

Sądowski

Belczyński

Bulik

et al. 2008

ApJ

Self Cite

127

157

View full text Add to dashboard Cite

Using a population synthesis approach, we compute the total merger rate in the local universe for double neutron stars, double black holes, and black hole-neutron star binaries. These compact binaries are the prime source candidates for gravitational wave detection by LIGO and VIRGO. We account for mergers originating both from field populations and from dense stellar clusters, where dynamical interactions can significantly enhance the production of double compact objects. For both populations we use the same treatment of stellar evolution. Our results indicate that the merger rates of double neutron stars and black hole-neutron star binaries are strongly dominated by field populations, while merging black hole binaries are formed much more effectively in dense stellar clusters. The overall merger rate of double compact objects depends sensitively on the (largely unknown) initial mass fraction contained in dense clusters ( f cl ). For f cl P 0:0001, the Advanced LIGO detection rate will be dominated by field populations of double neutron star mergers, with a small but significant number of detections, $20 yr À1 . However, for a higher mass fraction in clusters, f cl k 0:001, the detection rate will be dominated by numerous mergers of double black holes originating from dense clusters, and it will be considerably higher, $25-300 yr À1 . In addition, we show that, once mergers of double black holes are detected, it is easy to differentiate between systems formed in the field and in dense clusters, since the chirp mass distributions are strikingly different. If significant field populations of double black hole mergers are detected, this will also place very strong constraints on common-envelope evolution in massive binaries. Finally, we point out that there may exist a population of merging black hole binaries in intergalactic space.

show abstract

Binary Mergers and Growth of Black Holes in Dense Star Clusters

Cited by 306 publications

References 60 publications

Search for gravitational waves from intermediate mass binary black holes

Search for gravitational waves from intermediate mass binary black holes

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

The Total Merger Rate of Compact Object Binaries in the Local Universe

Contact Info

Product

Resources

About