PALFA Discovery of a Highly Relativistic Double Neutron Star Binary

Stovall, K.; Freire, P. C. C.; Chatterjee, Shami; Demorest, Paul; Lorimer, D. R.; McLaughlin, M. A.; Pol, Nihan S.; Leeuwen, J. van; Wharton, Robert; Allen, B.; Boyce, M. M.; Brazier, A.; Caballero, K. S.; Camilo, F.; Camuccio, Richard; Cordes, J. M.; Crawford, F.; Deneva, J. S.; Ferdman, R. D.; Hessels, J. W. T.; Jenet, Fredrick; Kaspi, V. M.; Knispel, Benjamin; Lazarus, P.; Lynch, R.; Parent, E.; Patel, C.; Pleunis, Ziggy; Ransom, S. M.; Scholz, Paul; Seymour, A.; Siemens, X.; Stairs, I. H.; Swiggum, Joseph K.; Zhu, Weiwei

doi:10.3847/2041-8213/aaad06

Cited by 157 publications

(107 citation statements)

References 49 publications

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“…Since the discovery of the first neutron star -neutron star (NS-NS) binary, PSR B1913+16 (Hulse & Taylor 1975), 20 NS-NSs have been observed in the radio band in our Milky Way Galaxy alone (Tauris et al 2017, and references therein;Martinez et al 2017;Cameron et al 2018;Lynch et al 2018;Stovall et al 2018;Ridolfi et al 2019). More recently, the first gravitational-wave signal from a NS-NS merger, GW170817, was detected by the Advanced LIGO/Virgo network (Abbott et al 2017).…”

Section: Introductionmentioning

confidence: 99%

On the Rate of Neutron Star Binary Mergers from Globular Clusters

Fong

Kremer

et al. 2019

ApJL

182

134

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The first detection of gravitational waves from a neutron star -neutron star (NS-NS) merger, GW170817, and the increasing number of observations of short gamma-ray bursts (SGRBs) have greatly motivated studies of the origins of NS-NS and neutron star -black hole (NS-BH) binaries. We calculate the merger rates of NS-NS and NS-BH binaries from globular clusters (GCs) using realistic GC simulations with the CMC cluster catalog. We use a large sample of models with a range of initial numbers of stars, metallicities, virial radii and galactocentric distances, representative of the present-day Milky Way GCs, to quantify the inspiral times and volumetric merger rates as a function of redshift, both inside and ejected from clusters. We find that over the complete lifetime of most GCs, stellar BHs dominate the cluster cores and prevent the mass segregation of NSs, thereby reducing the dynamical interaction rates of NSs so that at most a few NS binary mergers are ever produced. We estimate the merger rate in the local universe to be ∼ 0.02 Gpc −3 yr −1 for both NS-NS and NS-BH binaries, or a total of ∼ 0.04 Gpc −3 yr −1 for both populations. These rates are about 5 orders of magnitude below the current empirical merger rate from LIGO/Virgo. We conclude that dynamical interactions in GCs do not play a significant role in enhancing the NS-NS and NS-BH merger rates.

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Section: Introductionmentioning

confidence: 99%

On the Rate of Neutron Star Binary Mergers from Globular Clusters

Fong

Kremer

et al. 2019

ApJL

182

134

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“…Observed pulsars in Milky Way DNSs. References: a (Breton et al 2008;Ferdman et al 2013), b (Cameron et al 2018), c (Champion et al 2004), d (Faulkner et al 2004;Ferdman et al 2014), e (Nice et al 1996;Janssen et al 2008), f (Lazarus et al 2016Ferdman 2017), g (Lyne et al 2000;Corongiu et al 2006), h (Martinez et al 2015), i (Martinez et al 2017), j (Stovall et al 2018), k (Swiggum et al 2015), l (Fonseca et al 2014), m (Lynch et al 2018), n (Hulse & Taylor 1975;Weisberg & Huang 2016), o (Keith et al 2009), p (Ng et al 2018a), q (van Leeuwen et al 2015, r (Lynch et al 2012), s (Anderson et al 1990). Systems marked * are in globular clusters, whereas systems marked † may contain a white dwarf companion.…”

Section: Introductionmentioning

confidence: 99%

Modelling double neutron stars: radio and gravitational waves

Chattopadhyay

Stevenson

Hurley

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We have implemented prescriptions for modelling pulsars in the rapid binary population synthesis code COMPAS. We perform a detailed analysis of the double neutron star (DNS) population, accounting for radio survey selection effects. The surface magnetic field decay timescale (≈1000 Myr) and mass scale (≈0.02 M ) are the dominant uncertainties in our model. Mass accretion during common envelope evolution plays a non-trivial role in recycling pulsars. We find a best-fit model that is in broad agreement with the observed Galactic DNS population. Though the pulsar parameters (period and period derivative) are strongly biased by radio selection effects, the observed orbital parameters (orbital period and eccentricity) closely represent the intrinsic distributions. The number of radio observable DNSs in the Milky Way at present is ≈ 2500 in our model, only ≈ 10% of the predicted total number of DNSs in the galaxy. Using our model calibrated to the Galactic DNS population, we make predictions for DNS mergers observed in gravitational waves. The DNS chirp mass distribution varies from ≈1.1M to ≈2.1M and median is obtained to be 1.14 M . The expected effective spin χ eff for isolated DNSs is 0.03 from our model. We predict that ≈34% of the current Galactic isolated DNSs will merge within a Hubble time, and have a median total mass of 2.7 M . Finally, we discuss implications for fast radio bursts and post-merger remnant gravitational-waves.

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“…Adapted from Krokow et al (2018). served populations of close double white dwarfs (Breedt et al 2017, Napiwotzki et al 2019) and double neutron stars (Tauris et al 2017, Stovall et al 2018, Andrews & Zezas 2019 have been evolving accordingly. Consequently, we may expect that also close double black holes from in a similar way.…”

Section: Introductionmentioning

confidence: 99%

Properties of OB star−black hole systems derived from detailed binary evolution models

Langer

Schürmann

Stoll

et al. 2020

A&A

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Context. The recent gravitational wave measurements have demonstrated the existence of stellar mass black hole binaries. It is essential for our understanding of massive star evolution to identify the contribution of binary evolution to the formation of double black holes. Aims. A promising way to progress is investigating the progenitors of double black hole systems and comparing predictions with local massive star samples such as the population in 30 Doradus in the Large Magellanic Cloud (LMC). Methods. To this purpose, we analyse a large grid of detailed binary evolution models at LMC metallicity with initial primary masses between 10 and 40 M , and identify which model systems potentially evolve into a binary consisting of a black hole and a massive main sequence star. We then derive the observable properties of such systems, as well as peculiarities of the OB star component. Results. We find that ∼3% of the LMC late O and early B stars in binaries are expected to possess a black hole companion, when assuming stars with a final helium core mass above 6.6 M to form black holes. While the vast majority of them may be X-ray quiet, our models suggest that these may be identified in spectroscopic binaries, either by large amplitude radial velocity variations ( ∼ > 50 km s −1 ) and simultaneous nitrogen surface enrichment, or through a moderate radial velocity ( ∼ > 10 km s −1 ) and simultaneously rapid rotation of the OB star. The predicted mass ratios are such that main sequence companions could be excluded in most cases. A comparison to the observed OB+WR binaries in the LMC, Be/X-ray binaries, and known massive BH binaries supports our conclusion. Conclusions. We expect spectroscopic observations to be able to test key assumptions in our models, with important implications for massive star evolution in general, and for the formation of double-black hole mergers in particular.

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PALFA Discovery of a Highly Relativistic Double Neutron Star Binary

Cited by 157 publications

References 49 publications

On the Rate of Neutron Star Binary Mergers from Globular Clusters

On the Rate of Neutron Star Binary Mergers from Globular Clusters

Modelling double neutron stars: radio and gravitational waves

Properties of OB star−black hole systems derived from detailed binary evolution models

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