Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant
© 2020 IOP Publishing Ltd. GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neut...
| Main Authors: | , |
|---|---|
| Other Authors: | |
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2021
|
| Online Access: | https://hdl.handle.net/1721.1/132423 |
| _version_ | 1826195182545010688 |
|---|---|
| author | LIGO Scientific Collaboration Virgo Collaboration |
| author2 | LIGO (Observatory : Massachusetts Institute of Technology) |
| author_facet | LIGO (Observatory : Massachusetts Institute of Technology) LIGO Scientific Collaboration Virgo Collaboration |
| author_sort | LIGO Scientific Collaboration |
| collection | MIT |
| description | © 2020 IOP Publishing Ltd. GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05M⊙, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67M⊙ for the case that the merger results in a hypermassive neutron star. |
| first_indexed | 2024-09-23T10:08:40Z |
| format | Article |
| id | mit-1721.1/132423 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T10:08:40Z |
| publishDate | 2021 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1324232023-01-06T18:28:41Z Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant LIGO Scientific Collaboration Virgo Collaboration LIGO (Observatory : Massachusetts Institute of Technology) Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research © 2020 IOP Publishing Ltd. GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05M⊙, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67M⊙ for the case that the merger results in a hypermassive neutron star. 2021-09-20T18:22:18Z 2021-09-20T18:22:18Z 2020 2020-10-21T17:02:04Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/132423 en 10.1088/1361-6382/AB5F7C Classical and Quantum Gravity Creative Commons Attribution 3.0 unported license https://creativecommons.org/licenses/by/3.0/ application/pdf IOP Publishing The American Astronomical Society |
| spellingShingle | LIGO Scientific Collaboration Virgo Collaboration Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title | Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title_full | Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title_fullStr | Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title_full_unstemmed | Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title_short | Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant |
| title_sort | model comparison from ligo virgo data on gw170817 s binary components and consequences for the merger remnant |
| url | https://hdl.handle.net/1721.1/132423 |
| work_keys_str_mv | AT ligoscientificcollaboration modelcomparisonfromligovirgodataongw170817sbinarycomponentsandconsequencesforthemergerremnant AT virgocollaboration modelcomparisonfromligovirgodataongw170817sbinarycomponentsandconsequencesforthemergerremnant |