| Issue |
A&A
Volume 639, July 2020
|
|
|---|---|---|
| Article Number | A123 | |
| Number of page(s) | 6 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202037519 | |
| Published online | 22 July 2020 | |
Masses of double neutron star mergers
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China
e-mail: mkruckow@ynao.ac.cn
Received:
17
January
2020
Accepted:
27
May
2020
Aims. I aim to explain the mass discrepancy between the observed double neutron-star binary population by radio pulsar observations and gravitational-wave observation.
Methods. I performed binary population synthesis calculations and compared their results with the radio and the gravitational-wave observations simultaneously.
Results. Simulations of binary evolution were used to link different observations of double neutron star binaries with each other. I investigated the progenitor of GW190425 in more detail. A distribution of masses and merger times of the possible progenitors is presented.
Conclusions. A mass discrepancy between the radio pulsars in the Milky Way with another neutron star companion and the inferred masses from gravitational-wave observations of those kind of merging systems is naturally found in binary evolution.
Key words: binaries: close / gravitational waves / pulsars: general / stars: neutron / stars: evolution
© ESO 2020
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