Galactic distribution of merging neutron stars and black holes – prospects for short gamma-ray burst progenitors and LIGO/VIRGO

By R. Voss, T. Tauris. 2003

200 citations recorded by the source corpus.

We have performed a detailed population synthesis on a large number (2 x 10 7 ) of binary systems in order to investigate the properties of massive double degenerate binaries. We have included new important results in ourinput physics in order to obtain more reliable estimates of the merging time-scales and relative formation rates. These improvements include refined treatment of the binding energy in a common envelope, helium star evolution and reduced kicks imparted to new-born black holes. The discovery and observations of gamma-ray burst afterglows and the identification of host galaxies have allowed comparisons of theoretical distributions of merger sites with the observed distribution of afterglow positions relative to host galaxies. To help investigate the physical nature of short- and long-duration gamma-ray bursts, we compute the distances of merging neutron stars (NS) and/or black holes (BH) from the centres of their host galaxies, as predicted by their formation scenario combined with motion in galactic potentials. Furthermore, we estimate the formation rate and merging rate of these massive double degenerate binaries. The latter is very important for the prospects of detecting gravitational waves with LIGO/VIRGO. We find that the expected detection rate for LIGO II is ∼850 yr - 1 for galactic field sources and that this rate is completely dominated by merging double black hole (BHBH) binaries. Even LIGO I may detect such an event (∼0.25 yr - 1 ). Our preferred model estimates the Galactic field double neutron star (NSNS) merger rate to be ∼1.5 × 10 - 6 yr - 1 . For BHBH systems this model predicts a merger rate of ∼9.7 x 10 - 6 yr - 1 . Our studies also reveal an accumulating numerous population of very wide-orbit BHBH systems which never merge (τ >> τ H u b b l e ).

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/dc7f58f22bcb9b3a5147de1d6e977d0f9a6fff03

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1. Michela Mapelli
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Citations in the corpus

• DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES (2015, unknown): “…Lipunov et al. 1997; Bethe & Brown 1998; De Donder & Vanbeveren 1998, 2004a; Bloom et al. 1999; Grishchuk et al. 2001; Nelemans et al. 2001; Dewi & Pols 2003; Voss & Tauris 2003a; Nutzman et al. 2004; Pfahl et al. 2005; Postnov & Yungelson 2006; Marassi et al. 2011; Mennekens & Vanbeveren 2014).”
• Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, unknown): “…include Lipunov et al. (1997); Bethe & Brown (1998); Bloom et al. (1999); De Donder & Vanbeveren (2004); Grishchuk et al. (2001); Nelemans (2003); Voss & Tauris (2003); Pfahl et al. (2005); Dewi et al. (2006); O’Shaughnessy et al. (2008); Mennekens & Vanbeveren (2014); Dominik et al. (2015); de…”
• ILLUMINATING BLACK HOLE BINARY FORMATION CHANNELS WITH SPINS IN ADVANCED LIGO (2016, background): “…two categories: the “field” channel, in which BBHs are formed from isolated stellar binaries, usually involving either a commonenvelope phase (e.g., Voss & Tauris 2003; Dominik et al. 2012, 2013; Belczynski et al. 2016) or chemicallyhomogeneous evolution due to rapid stellar rotation (e.g. De…”
• Double neutron stars: merger rates revisited (2017, background): “This is generally found to increase the rates by a factor of a few (e.g. Voss & Tauris 2003; Dominik et al. 2012; Mennekens & Vanbeveren 2014; Chruslinska et al. 2017, except for Bogomazov et al. (2007) who find the increase even greater than an order of magnitude, however, when they allow for the…”
• Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…the galactic field through common-envelope evolution(Bethe & Brown 1998; Portegies Zwart & Yungelson 1998; Belczynski et al. 2002, 2007, 2008, 2014; Voss & Tauris 2003; Dewi et al. 2006; Dominik et al. 2013; Mennekens & Vanbeveren 2014; Spera et al. 2015; Eldridge & Stanway 2016; Mapelli et al.…”
• Ultra-stripped supernovae: progenitors and fate (2015, methodology): “Therefore, to ensure survival of these systems, the first SN must have imparted a small kick on the newborn NS, less than200 km s−1 and with an average of only∼ 50 kms−1 (Voss & Tauris 2003).”
• Binary Black Hole Mergers in the First Advanced LIGO Observing Run (2016, background): “[168–173]), possibly from population III binaries [174,175], or chemically homogeneous evolution in close tidally locked binaries [176,177].”
• Runaway stars as progenitors of supernovae and gamma-ray bursts (2011, background): “Black holes are not normally considered to have significant kicks although their importance has been investigated by others (Brandt, Podsiadlowski & Sigurdsson 1995; Kalogera 1999; Mirabel et al. 2002, 2004; Voss & Tauris 2003).”
• The chemically homogeneous evolutionary channel for binary black hole mergers: rates and properties of gravitational-wave events detectable by advanced LIGO (2016, background): “…predicted that the gravitational-wave signals of binary black hole mergers would potentially dominate LIGO observations (e.g. Lipunov et al. 1997; Voss & Tauris 2003; Belczynski et al. 2010; Dominik et al. 2015), but these analyses also demonstrated the significant uncertainties in these…”
• The Origin of r-process Elements in the Milky Way (2017, background): “Population Synthesis Population synthesis models predict NS-NS merger rates for stellar populations (e.g., Fryer et al. 1999; Voss & Tauris 2003; Mennekens & Vanbeveren 2014; Dominik et al. 2012; Belczynski et al. 2016a; Chruslinska et al. 2017).”
• Formation of Double Neutron Star Systems (2017, background): “…can be combined with the merger time for the DNS system to estimate the offset distance of the future DNS merger (short GRB) from its birth place in the Galactic disk (e.g. Bloom et al. 1999; Perna & Belczynski 2002; Voss & Tauris 2003; Fong et al. 2010; Kelley et al. 2010; Beniamini et al. 2016b).”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “…of stars in a binary through mass transfer and a common envelope phase (Tutukov & Yungelson 1993; Lipunov et al. 1997; Belczynski et al. 2002; Voss & Tauris 2003; Dominik et al. 2012; Belczynski et al. 2016b; Eldridge & Stanway 2016; Woosley 2016; Stevenson et al. 2017; Kruckow et al. 2018;…”
• The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale (2017, background): “For example, the distribution of delay times (i.e., the sum of the evolutionary time to form a BNS system and its time to merge) is a key output of population synthesis simulations (e.g., Voss & Tauris 2003; Belczynski et al. 2006; Dominik et al. 2012).”
• Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, methodology): “…population studies performed with our code (= the Brussels code, De Donder and Vanbeveren, 1998, 2004a, b) predict almost no BH+BH or NS+BH mergers whereas in the simulations of Voss and Tauris (2003) the double BH mergers are about two orders of magnitude larger than the BH+NS and NS+NS mergers.”
• DOUBLE COMPACT OBJECTS. I. THE SIGNIFICANCE OF THE COMMON ENVELOPE ON MERGER RATES (2012, methodology): “Several different groups have provided similar estimates in the past decade (Nelemans et al., 2001; Voss & Tauris, 2003; Dewi & Pols, 2003; Nutzman et al., 2004; Pfahl et al., 2005), and exploration of the relevant physical processes and rate estimates were obtained with the StarTrack population…”
• Dynamics of stellar black holes in young star clusters with different metallicities – II. Black hole–black hole binaries (2014, methodology): “…Sigurdsson & Chernoff 2013), or in the field, using population synthesis simulations of isolated binaries (e.g. Belczynski, Kalogera & Bulik 2002; Voss & Tauris 2003; Pfahl, Podsiadlowski & Rappaport 2005; Dewi, Podsiadlowski & Sena 2006; Belczynski et al. 2007, 2010a; Dominik et al. 2012).”
• Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, methodology): “This question is not only relevant for interpreting observations, e.g. of hypervelocity stars (Tauris 2015), but also, for example, for stellar population studies and for understanding the evolution of binary stars that give birth to double NS systems (e.g. Voss & Tauris 2003; Tauris et al. 2016).”
• Hierarchical analysis of gravitational-wave measurements of binary black hole spin–orbit misalignments (2017, result): “These rates are broadly consistent with predictions from both population synthesis models of isolated binary evolution (e.g., Voss & Tauris 2003; Lipunov et al. 2009; Dominik et al. 2012; Postnov & Yungelson 2014) and dynamical formation models (e.g., Sigurdsson & Hernquist 1993; Sadowski et al.…”