Formation of Double Neutron Star Systems

By J. Antoniadis, Hailiang Chen, P. Freire, L. Guillemot, Jason W. T. Hessels, A. Istrate, Victoria Kaspi, M. Kramer, M. Kruckow, N. Langer and 12 more. 2017

433 citations recorded by the source corpus.

Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square Kilometre Array searching for radio pulsars, and the high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase, and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most . We investigate DNS masses, spins, and velocities, and in particular correlations between spin period, orbital period, and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes that may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/8b29b59b3226049819d00c736d401811780e3c5e

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Citations in the corpus

Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, methodology): “For ultra-stripped SNe this is motived by the kinematics of known double NS systems; see detailed discussions in Tauris et al. (2017).”
The effect of the metallicity-specific star formation history on double compact object mergers (2019, background): “If the progenitor either experiences an electron capture supernova or is ultrastripped by an NS companion, we lower the 1D root mean square kick to 30 km s−1 (Pfahl et al. 2002; Podsiadlowski et al. 2004; Tauris et al. 2015, 2017; VignaGómez 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, methodology): “This value is within the range of observed and simulated velocity distributions for Galactic BNS systems (Wong et al. 2010; Tauris et al. 2017).”
GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run (2020, methodology): “1 M⊙ is greater than that of observed Galactic BNSs [274,275].”
Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, methodology): “The total mass and mass ratio will be used for exploring the formation process of binary neutron stars(Tauris et al. 2017).”
Massive runaway and walkaway stars (2018, background): “Recently, multi-dimensional calculations of fallback in CC resulting in the formation of a BH found that large natal kicks might be possible (Chan et al. 2018).”
Merging black holes in young star clusters (2019, background): “…al. 2007, 2008; Bogomazov et al. 2007; Moody & Sigurdsson 2009; Dominik et al. 2012, 2013, 2015; Mapelli et al. 2013; Mennekens & Vanbeveren 2014; Tauris et al. 2015, 2017; de Mink & Belczynski 2015; de Mink & Mandel 2016; Marchant et al. 2016; Belczynski et al. 2016a; Chruslinska et al. 2018;…”
Rates of compact object coalescences (2021, background): “Nearly 20 such binaries have been observed in the Galaxy through radio pulsar pulsar observations (see, e.g., Tauris et al., 2017; Farrow et al., 2019, for recent compilations).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…al. 2006; Dominik et al. 2013; Mennekens & Vanbeveren 2014; Spera et al. 2015; Eldridge & Stanway 2016; Mapelli et al. 2017; Stevenson et al. 2017b; Tauris et al. 2017; Chruslinska et al. 2018; Giacobbo & Mapelli 2018; Giacobbo et al. 2018; Kruckow et al. 2018; Mapelli & Giacobbo 2018) or via…”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…to observational findings, e.g., on the distribution and systematics of neutron star birth masses (Özel & Freire 2016; Antoniadis et al. 2016; Tauris et al. 2017), neutron star kicks (Hobbs et al. 2005; Faucher-Giguère & Kaspi 2006; Ng & Romani 2007), and supernova explosion energies and…”
The cosmic merger rate of neutron stars and black holes (2018, background): “A possible physical interpretation is that the vast majority of DNSs form from ultrastripped SNe, which are expected to produce very small natal kicks (< 50 km s−1, Suwa et al. 2015; Tauris et al. 2015, 2017).”