The Cosmic Coalescence Rates for Double Neutron Star Binaries

By Vicky Kalogera, Chunglee Kim, D. R. Lorimer, M. Burgay, N. D’Amico, A. Possenti, R. Manchester, Andrew G. Lyne, B. C. Joshi, M. Mclaughlin and 3 more. 2003

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We report on the newly increased event rates due to the recent discovery of the highly relativistic binary pulsar J0737-3039. Using a rigorous statistical method, we present the calculations reported by Burgay et al., which produce a coalescence rate for Galactic double neutron star (DNS) systems that is higher by a factor of 6-7 compared to estimates made prior to the new discovery. Our method takes into account known pulsar survey selection effects and biases due to small-number statistics. This rate increase has dramatic implications for gravitational wave detectors. For the initial Laser Interferometer Gravitational-Wave Observatory (LIGO) detectors, the most probable detection rates for DNS in-spirals are one event per 5-250 yr; at 95% confidence, we obtain rates up to one per 1.5 yr. For the advanced LIGO detectors, the most probable rates are 20-1000 events per year. These predictions, for the first time, bring the expectations for DNS detections by the initial LIGO detectors to the astrophysically relevant regime. We also use our models to predict that the large-scale Parkes Multibeam pulsar survey with acceleration searches could detect an average of three to four binary pulsars similar to those known at present.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/26e6a6ab47b37842431d889ddfd633d02fbabc36

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Citations in the corpus

Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “The frequency of such events can be estimated on grounds of the known double NS systems in the solar neighbourhood (e.g. Kalogera et al. 2004) and theoretical population synthesis studies (e.g. Belczynski E-mail: ojust@mpa-garching.mpg.de et al. 2008) to be of the order of one NS–NS merger in some…”
The electromagnetic signals of compact binary mergers (2012, methodology): “Merger rate estimates based on these binaries (Kalogera et al. 2004a,b) suggest a comparable rate of events to the beaming corrected rate inferred from short GRBs.”
COMPACT BINARY MERGER RATES: COMPARISON WITH LIGO/VIRGO UPPER LIMITS (2015, background): “…N., et al. 2013, A&ARv, 21, 59 Janka, T. 2013, MNRAS, 434, 1355 Jin, Z., Li, X., Cano, Z., Covino, S., Fan, Y., Wei, D. 2015, ApJ, 811, L22 Juric, M., et al. 2008, ApJ, 673, 864 Justham, S., Rappaport, S., Podsiadlowski, P. 2006, MNRAS, 366, 1415 Kalogera et al. 2004, ApJ, 601, L179; erratum ibid.”
TOWARD EARLY-WARNING DETECTION OF GRAVITATIONAL WAVES FROM COMPACT BINARY COALESCENCE (2011, background): “The merger rates have substantial measurement uncertainty due to the small sample of known double pulsar systems that will merge within a Hubble time; they also have systematic uncertainty due to sensitive dependence on the pulsar luminosity distribution function (Kalogera et al. 2004).”
GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, unknown): “…release > 4×1046 erg. Refs: [1] Guetta & Della Valle 2007; [2] Soderberg et al. 2006; [3a] Nakar, Gal-Yam & Fox 2006; [3b] Coward et al. 2012; [4] Kalogera et al. 2004; [5] Ofek 2007; [6] Scannapieco & Bildsten 2005; [7] Li et al. 2011 [8] Lorimer et al. 2007; [9] Thornton et al. 2013. tion of…”
Short-Duration Gamma-Ray Bursts (2013, methodology): “In the context of compact object mergers, this value coincides with the middle of the range based on estimates from the Galactic NS-NS binary population and from population synthesis models (Kalogera et al. 2004, Abadie et al. 2010).”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South (2017, methodology): “Matching the derived Galactic r-process production rate requires kilonova ejecta masses in the range of 0.01–0.1Me (e.g., Fernández & Metzger 2016), if estimates of the binary neutron star merger rate from the Galactic neutron star population are correct (Kalogera et al. 2004; Kim et al. 2015).”
ACCELERATING COMPACT OBJECT MERGERS IN TRIPLE SYSTEMS WITH THE KOZAI RESONANCE: A MECHANISM FOR “PROMPT” TYPE Ia SUPERNOVAE, GAMMA-RAY BURSTS, AND OTHER EXOTICA (2010, background): “Similarly, the massive star birthrate, which is ap- 1 Alfred P. Sloan Fellow proximately equal to the Type-II supernova rate,∼ 105 Gpc−3 yr−1 (e.g., Horiuchi et al. 2009), is∼ 20− 600 times larger than the NS-NS merger rate (Kalogera et al. 2001, 2004ab; O’Shaughnessy et al. 2008).”
EARLY X-RAY AND OPTICAL AFTERGLOW OF GRAVITATIONAL WAVE BURSTS FROM MERGERS OF BINARY NEUTRON STARS (2012, unknown): “The rate inferred from the Galactic NS-NS systems has a wide range 2 − 2 × 104 Gpc−3 yr−1 (Phinney 1991; Kalogera et al. 2004; Abadie et al. 2010).”
On the formation history of Galactic double neutron stars (2018, background): “Rates inferred from Galactic binary pulsars are dominated by a few systems and are sensitive to the imperfectly known pulsar radio luminosity distribution (Kalogera et al. 2004).”
The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions (2012, background): “If ns mergers alone were responsible for all r-process material this would constrain their galactic rate to 7 × 10−5 M yr−1, right in the centre of the 95 per cent confidence interval derived from the observed ns2 binary distribution (Kalogera et al. 2004), see Fig.”