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

Sądowski, Aleksander; Belczyński, Krzysztof; Bulik, T.; Іванова, Наталя; Rasio, Frederic A.; O’Shaughnessy, R.

doi:10.1086/528932

Cited by 127 publications

(181 citation statements)

References 51 publications

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“…Figure 5 then illustrates the temporal evolution of the galactic double compact binary merger rates. The rates at present are then translated into LIGO II rates using the method and parameter values outlined by , which is very similar to, e.g., the procedure by Sadowski et al (2008). This detection horizon is taken from the official LIGO website 8 .…”

Section: Resultsmentioning

confidence: 99%

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Mennekens

Vanbeveren

2014

A&A

172

197

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With our galactic evolutionary code that contains a detailed intermediate-mass and massive binary population model, we study the temporal evolution of the galactic population of double neutron star binaries, mixed systems with a neutron star and black hole component, and double black hole binaries. We computed the merger rates of these relativistic binaries and translate them into LIGO II detection rates. We demonstrate that accounting for the uncertainties in the relation "initial mass-final mass" predicted by massive close binary evolution and due to the possible effect of large stellar wind mass loss during the luminous blue variable phase of a star with initial mass higher than 30−40 M and during the red supergiant phase of a star with initial mass lower than 30−40 M when such a star is a binary component, the double black hole merger rate may be very low, contrary to predictions made by other groups. Hydrodynamic computations of the r-process chemical yields ejected during the relativistic binary merger process have recently become available. With our galactic code that includes binaries, it is then straightforward to calculate the temporal galactic evolution of the r-process elements ejected by these mergers. We conclude that except for the earliest evolutionary phase of the Galaxy (∼the first 100 Myr), double compact star mergers may be the major production sites of r-process elements, and it is probable that the mixed systems dominate this production over double neutron star binary mergers.

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Section: Resultsmentioning

confidence: 99%

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Mennekens

Vanbeveren

2014

A&A

172

197

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“…On the one hand, the fraction of binaries and their orbital parameter distributions are the tracers of massive star formation and of the early dynamical evolution of their host star cluster. On the other hand, they determine the frequency of evolved massive binary systems, including highmass X-ray and double compact binaries (Sadowski et al 2008), Type Ib/c supernovae (Yoon et al 2010), short and long-duration gamma-ray bursts (Podsiadlowski et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The VLT-FLAMES Tarantula Survey

Sana

Koter

Mink

et al. 2013

A&A

501

605

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Context. The Tarantula Nebula in the Large Magellanic Cloud is our closest view of a starburst region and is the ideal environment to investigate important questions regarding the formation, evolution and final fate of the most massive stars. Aims. We analyze the multiplicity properties of the massive O-type star population observed through multi-epoch spectroscopy in the framework of the VLT-FLAMES Tarantula Survey. With 360 O-type stars, this is the largest homogeneous sample of massive stars analyzed to date. Methods. We use multi-epoch spectroscopy and variability analysis to identify spectroscopic binaries. We also use a Monte-Carlo method to correct for observational biases. By modeling simultaneously the observed binary fraction, the distributions of the amplitudes of the radial velocity variations and the distribution of the time scales of these variations, we constrain the intrinsic current binary fraction and period and mass-ratio distributions. Results. We observe a spectroscopic binary fraction of 0.35±0.03, which corresponds to the fraction of objects displaying statistically significant radial velocity variations with an amplitude of at least 20 km s −1 . We compute the intrinsic binary fraction to be 0.51±0.04. We adopt power-laws to describe the intrinsic period and mass-ratio distributions: f (log 10 P/d) ∼ (log 10 P/d) π (with log 10 P/d in the range 0.15−3.5) and f (q) ∼ q κ with 0.1 ≤ q = M 2 /M 1 ≤ 1.0. The power-law indexes that best reproduce the observed quantities are π = −0.45 ± 0.30 and κ = −1.0 ± 0.4. The period distribution that we obtain thus favours shorter period systems compared to an Öpik law (π = 0). The mass ratio distribution is slightly skewed towards low mass ratio systems but remains incompatible with a random sampling of a classical mass function (κ = −2.35). The binary fraction seems mostly uniform across the field of view and independent of the spectral types and luminosity classes. The binary fraction in the outer region of the field of view (r > 7.8 , i.e. ≈117 pc) and among the O9.7 I/II objects are however significantly lower than expected from statistical fluctuations. The observed and intrinsic binary fractions are also lower for the faintest objects in our sample (K s > 15.5 mag), which results from observational effects and the fact that our O star sample is not magnitude-limited but is defined by a spectral-type cutoff. We also conclude that magnitude-limited investigations are biased towards larger binary fractions. Conclusions. Using the multiplicity properties of the O stars in the Tarantula region and simple evolutionary considerations, we estimate that over 50% of the current O star population will exchange mass with its companion within a binary system. This shows that binary interaction is greatly affecting the evolution and fate of massive stars, and must be taken into account to correctly interpret unresolved populations of massive stars. Full Tables 1-3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

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“…Additional formation channels of BHBH in globular clusters have been investigated by O'Leary et al (2007), Sadowski et al (2008), and their dependence on metallicity has been explored by Ziosi et al (2014).…”

Section: Introductionmentioning

confidence: 99%

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

Kowalska-Leszczynska

Regimbau

Bulik

et al. 2015

A&A

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Context. Recent studies on stellar evolution have shown that the properties of compact objects strongly depend on the metallicity of the environment in which they were formed. Aims. Using some very simple assumptions on the metallicity of the stellar populations, we explore how this property affects the unresolved gravitational-wave background from extragalactic compact binaries. Methods. We obtained a suit of models using population synthesis code, estimated the gravitational-wave background they produce, and discuss its detectability with second-(advanced LIGO, advanced Virgo) and third-(Einstein Telescope) generation detectors. Results. Our results show that the background is dominated by binary black holes for all considered models in the frequency range of terrestrial detectors, and that it could be detected in most cases by advanced LIGO/Virgo, and with Einstein Telescope with a very high signal-to-noise ratio. The observed peak in a gravitational-wave spectrum depends on the metallicity of the stellar population.

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

Cited by 127 publications

References 51 publications

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Massive double compact object mergers: gravitational wave sources and r-process element production sites

The VLT-FLAMES Tarantula Survey

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

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