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Formation of Double Neutron Star Systems

Thomas M. TaurisMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyMichael KramerMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyP. C. C. FreireMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyNorbert WexMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyHans‐Thomas JankaMax Planck Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85748 Garching, GermanyN. LangerArgelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, GermanyPhilipp PodsiadlowskiDepartment of Astronomy, Oxford University, Oxford OX1 3RH, UKE. BozzoISDC Data Centre for Astrophysics, Chemin dEcogia 16, CH-1290 Versoix, SwitzerlandS. ChatyLaboratoire AIM (UMR 7158 CEA/DSM-CNRS-Université Paris Diderot), Irfu/Service d'Astrophysique, Centre de Saclay, F-91191 Gif-sur-Yvette Cedex, FranceMatthias U. KruckowArgelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, GermanyE. P. J. van den HeuvelAstronomical Institute Anton Pannekoek, University of Amsterdam, P.O. Box 94249, 1090 GE Amsterdam, The NetherlandsJohn AntoniadisDunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, CanadaR. P. BretonJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UKD. J. ChampionMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

2017en

ABI

Annotatsiya

Abstract 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.

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DOI: 10.3847/1538-4357/aa7e89

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