| Article | |
| Report number | arXiv:1711.02644 ; CERN-TH-2017-236 |
| Title | Gravitational-wave constraints on the neutron-star-matter Equation of State |
| Author(s) | Annala, Eemeli (Helsinki U. ; Helsinki Inst. of Phys.) ; Gorda, Tyler (Helsinki U. ; Helsinki Inst. of Phys.) ; Kurkela, Aleksi (CERN ; Stavanger U.) ; Vuorinen, Aleksi (Helsinki U. ; Helsinki Inst. of Phys.) |
| Publication | 2018-04-26 |
| Imprint | 2017-11-07 |
| Number of pages | 5 |
| Note | 6 pages, 4 figures; v2: results and discussion updated, version accepted to PRL |
| In: | Phys. Rev. Lett. 120 (2018) 172703 |
| DOI | 10.1103/PhysRevLett.120.172703 |
| Subject category | nucl-th ; Nuclear Physics - Theory ; hep-ph ; Particle Physics - Phenomenology ; astro-ph.HE ; Astrophysics and Astronomy |
| Abstract | The LIGO/Virgo detection of gravitational waves originating from a neutron-star merger, GW170817, has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter Equations of State (EoSs) that interpolate between state-of-the-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EoSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that smallest allowed tidal deformability of a similar-mass star is $\Lambda(1.4 M_\odot) = 120$. |
| Copyright/License | arXiv nonexclusive-distrib. 1.0 publication: © 2018 The Authors (License: CC-BY-4.0) |
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Záznam vytvorený 2017-12-14, zmenený 2024-08-06
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