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Great Impostors: Extremely Compact, Merging Binary Neutron Stars in the Mass Gap Posing as Binary Black Holes

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Great Impostors: Extremely Compact, Merging Binary Neutron Stars in the Mass Gap Posing as Binary Black Holes

dc.contributor.author	Tsokaros, Antonios
dc.contributor.author	Ruiz Meneses, Milton Javier
dc.contributor.author	Shapiro, Stuart L.
dc.contributor.author	Sun, Lunan
dc.contributor.author	Uryū, Kōji
dc.date.accessioned	2023-06-02T13:47:16Z
dc.date.available	2023-06-02T13:47:16Z
dc.date.issued	2020
dc.identifier.citation	Tsokaros, Antonios Ruiz Meneses, Milton Javier Shapiro, Stuart L. Sun, Lunan Ury&#363, K&#333ji 2020 Great Impostors: Extremely Compact, Merging Binary Neutron Stars in the Mass Gap Posing as Binary Black Holes Physical Review Letters 124 7 071101-1 071101-6
dc.identifier.uri	https://hdl.handle.net/10550/87671
dc.description.abstract	Can one distinguish a binary black hole undergoing a merger from a binary neutron star if the individual compact companions have masses that fall inside the so-called mass gap of 3-5 M⊙? For neutron stars, achieving such masses typically requires extreme compactness and in this work we present initial data and evolutions of binary neutron stars initially in quasiequilibrium circular orbits having a compactness C=0.336. These are the most compact, nonvacuum, quasiequilibrium binary objects that have been constructed and evolved to date, including boson stars. The compactness achieved is only slightly smaller than the maximum possible imposed by causality, Cmax=0.355, which requires the sound speed to be less than the speed of light. By comparing the emitted gravitational waveforms from the late inspiral to merger and postmerger phases between such a binary neutron star vs a binary black hole of the same total mass we identify concrete measurements that serve to distinguish them. With that level of compactness, the binary neutron stars exhibit no tidal disruption up until merger, whereupon a prompt collapse is initiated even before a common core forms. Within the accuracy of our simulations the black hole remnants from both binaries exhibit ringdown radiation that is not distinguishable from a perturbed Kerr spacetime. However, their inspiral leads to phase differences of the order of ∼5 rad over an ∼81 km separation (1.7 orbits) while typical neutron stars exhibit phase differences of ≥20 rad. Although a difference of ∼5 rad can be measured by current gravitational wave laser interferometers (e.g., aLIGO/Virgo), uncertainties in the individual masses and spins will likely prevent distinguishing such compact, massive neutron stars from black holes.
dc.language.iso	eng
dc.relation.ispartof	Physical Review Letters, 2020, vol. 124, num. 7, p. 071101-1-071101-6
dc.subject	Astrofísica
dc.title	Great Impostors: Extremely Compact, Merging Binary Neutron Stars in the Mass Gap Posing as Binary Black Holes
dc.type	journal article
dc.date.updated	2023-06-02T13:47:17Z
dc.identifier.doi	10.1103/PhysRevLett.124.071101
dc.identifier.idgrec	160087
dc.rights.accessRights	open access