The Impact of Finite-Differencing Errors on Binary Black Hole Merger Templates

2006 ◽  
Author(s):  
Birjoo Vaishnav ◽  
Deirdre Shoemaker ◽  
Shane Larson
Keyword(s):  
Black Hole ◽  
Finite Differencing ◽  
Binary Black Hole ◽  
The Impact

scholarly journals Erratum: Binary black hole mergers from globular clusters: the impact of globular cluster properties

2019 ◽  
Vol 491 (4) ◽  
pp. 5793-5793
Author(s):  
Jongsuk Hong ◽  
Enrico Vesperini ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Magdalena Szkudlarek ◽  
...  
Keyword(s):  
Black Hole ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Binary Black Hole ◽  
Cluster Properties ◽  
The Impact

scholarly journals The Impact of Pair-instability Mass Loss on the Binary Black Hole Mass Distribution

2019 ◽  
Vol 882 (2) ◽  
pp. 121 ◽  
Author(s):  
Simon Stevenson ◽  
Matthew Sampson ◽  
Jade Powell ◽  
Alejandro Vigna-Gómez ◽  
Coenraad J. Neijssel ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Loss ◽  
Mass Distribution ◽  
Black Hole Mass ◽  
Binary Black Hole ◽  
The Impact

scholarly journals The effect of the metallicity-specific star formation history on double compact object mergers

2019 ◽  
Vol 490 (3) ◽  
pp. 3740-3759 ◽  
Author(s):  
Coenraad J Neijssel ◽  
Alejandro Vigna-Gómez ◽  
Simon Stevenson ◽  
Jim W Barrett ◽  
Sebastian M Gaebel ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Black Hole ◽  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Compact Object ◽  
Star Formation History ◽  
Binary Black Hole ◽  
Binary Evolution ◽  
The Impact

ABSTRACT We investigate the impact of uncertainty in the metallicity-specific star formation rate over cosmic time on predictions of the rates and masses of double compact object mergers observable through gravitational waves. We find that this uncertainty can change the predicted detectable merger rate by more than an order of magnitude, comparable to contributions from uncertain physical assumptions regarding binary evolution, such as mass transfer efficiency or supernova kicks. We statistically compare the results produced by the COMPAS population synthesis suite against a catalogue of gravitational-wave detections from the first two Advanced LIGO and Virgo observing runs. We find that the rate and chirp mass of observed binary black hole mergers can be well matched under our default evolutionary model with a star formation metallicity spread of 0.39 dex around a mean metallicity 〈Z〉 that scales with redshift z as 〈Z〉 = 0.035 × 10−0.23z, assuming a star formation rate of $0.01 \times (1+z)^{2.77} / (1+((1+z)/2.9)^{4.7}) \, \rm {M}_\odot$ Mpc−3 yr−1. Intriguingly, this default model predicts that 80 per cent of the approximately one binary black hole merger per day that will be detectable at design sensitivity will have formed through isolated binary evolution with only dynamically stable mass transfer, i.e. without experiencing a common-envelope event.

scholarly journals The impact of mass-transfer physics on the observable properties of field binary black hole populations

2021 ◽  
Author(s):  
S. S. Bavera ◽  
T. Fragos ◽  
M. Zevin ◽  
C. P. L. Berry ◽  
P. Marchant ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Black Hole ◽  
Binary Black Hole ◽  
The Impact

scholarly journals Reducing phase error in long numerical binary black hole evolutions with sixth-order finite differencing

2008 ◽  
Vol 25 (10) ◽  
pp. 105006 ◽  
Author(s):  
Sascha Husa ◽  
José A González ◽  
Mark Hannam ◽  
Bernd Brügmann ◽  
Ulrich Sperhake
Keyword(s):  
Black Hole ◽  
Phase Error ◽  
Sixth Order ◽  
Finite Differencing ◽  
Binary Black Hole

scholarly journals Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates

2021 ◽  
Vol 922 (2) ◽  
pp. 110
Author(s):  
Monica Gallegos-Garcia ◽  
Christopher P L Berry ◽  
Pablo Marchant ◽  
Vicky Kalogera
Keyword(s):  
Mass Transfer ◽  
Black Holes ◽  
Black Hole ◽  
Stellar Structure ◽  
Dynamical Instability ◽  
Population Synthesis ◽  
Binary Black Holes ◽  
Common Envelope ◽  
Binary Black Hole ◽  
The Impact

Abstract Rapid binary population synthesis codes are often used to investigate the evolution of compact-object binaries. They typically rely on analytical fits of single-star evolutionary tracks and parameterized models for interactive phases of evolution (e.g., mass transfer on a thermal timescale, determination of dynamical instability, and common envelope) that are crucial to predict the fate of binaries. These processes can be more carefully implemented in stellar structure and evolution codes such as MESA. To assess the impact of such improvements, we compare binary black hole mergers as predicted in models with the rapid binary population synthesis code COSMIC to models ran with MESA simulations through mass transfer and common-envelope treatment. We find that results significantly differ in terms of formation paths, the orbital periods and mass ratios of merging binary black holes, and consequently merger rates. While common-envelope evolution is the dominant formation channel in COSMIC, stable mass transfer dominates in our MESA models. Depending upon the black hole donor mass, and mass-transfer and common-envelope physics, at subsolar metallicity, COSMIC overproduces the number of binary black hole mergers by factors of 2–35 with a significant fraction of them having merger times orders of magnitude shorter than the binary black holes formed when using detailed MESA models. Therefore we find that some binary black hole merger rate predictions from rapid population syntheses of isolated binaries may be overestimated by factors of ∼ 5–500. We conclude that the interpretation of gravitational-wave observations requires the use of detailed treatment of these interactive binary phases.

scholarly journals Binary black hole mergers from globular clusters: the impact of globular cluster properties

2018 ◽  
Vol 480 (4) ◽  
pp. 5645-5656 ◽  
Author(s):  
Jongsuk Hong ◽  
Enrico Vesperini ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Magdalena Szkudlarek ◽  
...  
Keyword(s):  
Black Hole ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Binary Black Hole ◽  
Cluster Properties ◽  
The Impact
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