Publication: Was GW170817 a Canonical Neutron Star Merger? Bayesian Analysis with a Third Family of Compact Stars
| dc.contributor.author | Blaschke, D. | |
| dc.contributor.author | Ayriyan, A. | |
| dc.contributor.author | Alvarez-Castillo, D. E. | |
| dc.contributor.author | Grigorian, H. | |
| dc.date.accessioned | 2024-11-26T15:29:42Z | |
| dc.date.available | 2024-11-26T15:29:42Z | |
| dc.date.issued | 2020 | |
| dc.description.abstract | We investigate the possibility that GW170817 was not the merger of two conventional neutron stars (NS), but involved at least one if not two hybrid stars with a quark matter core that might even belong to a third family of compact stars. To this end, we develop a Bayesian analysis method for selecting the most probable equation of state (EoS) under a set of constraints from compact star physics, which now also include the tidal deformability from GW170817 and the first result for the mass and radius determination for PSR J0030+0451 by the NICER Collaboration. We apply this method for the first time to a two-parameter family of hybrid EoS based on the DD2 model with nucleonic excluded volume for hadronic matter and the color superconducting generalized nlNJL model for quark matter. The model has a variable onset density for deconfinement and can mimic the effects of pasta phases with the possibility of producing a third family of hybrid stars in the mass-radius diagram. The main findings of this study are that: (1) the presence of multiple configurations for a given mass (twins or even triples) corresponds to a set of disconnected lines in the Lambda(1)-Lambda(2) diagram of tidal deformabilities for binary mergers, so that merger events from the same mass range may result in a probability landscape with different peak positions; (2) the Bayesian analysis with the above observational constraints favors an early onset of the deconfinement transition, at masses of M-onset <= 0.8 M-circle dot with an M-R relationship that in the range of observed neutron star masses is almost indistinguishable from that of a soft hadronic Akmal, Pandharipande, and Ravenhall (APR) EoS; (3) a few, yet fictitious measurements of the NICER experiment two times more accurate than the present value and a different mass and radius that would change the posterior likelihood so that hybrid EoS with a phase transition onset in the range M-onset = 1.1-1.6 M-circle dot would be favored. | |
| dc.identifier.citation | Was GW170817 a Canonical Neutron Star Merger? Bayesian Analysis with a Third Family of Compact Stars / Blaschke, D [et al.] // Universe. - 2020. - 6. - № 6. - 10.3390/universe6060081 | |
| dc.identifier.doi | 10.3390/universe6060081 | |
| dc.identifier.uri | https://www.doi.org/10.3390/universe6060081 | |
| dc.identifier.uri | https://www.scopus.com/record/display.uri?eid=2-s2.0-85090245413&origin=resultslist | |
| dc.identifier.uri | http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcAuth=Alerting&SrcApp=Alerting&DestApp=WOS_CPL&DestLinkType=FullRecord&UT=WOS:000551095300005 | |
| dc.identifier.uri | https://openrepository.mephi.ru/handle/123456789/22110 | |
| dc.relation.ispartof | Universe | |
| dc.title | Was GW170817 a Canonical Neutron Star Merger? Bayesian Analysis with a Third Family of Compact Stars | |
| dc.type | Article | |
| dspace.entity.type | Publication | |
| oaire.citation.issue | 6 | |
| oaire.citation.volume | 6 | |
| relation.isOrgUnitOfPublication | dcdb137c-0528-46a5-841b-780227a67cce | |
| relation.isOrgUnitOfPublication.latestForDiscovery | dcdb137c-0528-46a5-841b-780227a67cce |