Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 481, Issue 3, Pages 4009-4029Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty2463
Keywords
binaries: general; stars: neutron; pulsars: general
Categories
Funding
- Consejo Nacional de Ciencia y Tecnologia (CONACYT)
- PHAROS European Cooperation in Science and Technology (COST) Action [CA16214]
- Science and Technology Facilities Council (STFC)
- Polish National Science Center (NCN) [DEC-2012/07/E/ST9/01360, 2015/19/B/ST9/01099]
- Strategic Priority Research Program of the Chinese Academy of Sciences 'Multi-waveband Gravitational Wave Universe' [XDB23040000]
- Chinese Academy of Sciences [2011Y2JB07]
- National Natural Science Foundation of China [11633005]
- European Union's Horizon 2020 research and innovation programme from the European Research Council (ERC) [GS100010663]
- National Science Foundation [NSF PHY11-25915]
- Australian Research Council (ARC) through ARC Future Fellowship [FT160100035]
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery [CE170100004]
- Kavli Foundation
- Danish National Research Foundation (DNRF)
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Double neutron stars (DNSs) have been observed as Galactic radio pulsars, and the recent discovery of gravitational waves from the DNS merger GW170817 adds to the known DNS population. We perform rapid population synthesis of massive binary stars and discuss model predictions, including DNS formation rates, mass distributions, and delay time distributions. We vary assumptions and parameters of physical processes such as mass transfer stability criteria, supernova natal kick distributions, remnant mass prescriptions, and common-envelope energetics. We compute the likelihood of observing the orbital period-eccentricity distribution of the Galactic DNS population under each of our population synthesis models, allowing us to quantitatively compare the models. We find that mass transfer from a stripped post-helium-burning secondary (case BB) on to a neutron star is most likely dynamically stable. We also find that a natal kick distribution composed of both low (Maxwellian sigma = 30 km s(-1)) and high (sigma = 265 km s(-1)) components is preferred over a single high-kick component. We conclude that the observed DNS mass distribution can place strong constraints on model assumptions.
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