Journal
PHYSICAL REVIEW LETTERS
Volume 121, Issue 16, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.121.161101
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Funding
- Council of Scientific and Industrial Research of India
- Department of Science and Technology, India
- Science AMP
- Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Agencia Estatal de Investigacion
- Vicepresidencia i Conselleria d'Innovacio, Recerca i Turisme
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears
- Conselleria d'Educacio, Investigacio, Cultura i Esport de la Generalitat Valenciana
- National Science Centre of Poland
- Swiss National Science Foundation (SNSF)
- Russian Foundation for Basic Research
- Russian Science Foundation
- European Commission
- European Regional Development Funds (ERDF)
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- Lyon Institute of Origins (LIO)
- Paris Ile-de-France Region
- National Research, Development and Innovation Office Hungary (NKFI)
- National Research Foundation of Korea
- Province of Ontario through the Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council Canada
- Canadian Institute for Advanced Research
- Brazilian Ministry of Science, Technology, Innovations, and Communications
- Research Grants Council of Hong Kong
- National Natural Science Foundation of China (NSFC)
- Leverhulme Trust
- Research Corporation
- Ministry of Science and Technology (MOST), Taiwan
- Kavli Foundation
- Industry Canada
- International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
- U.S. National Science Foundation (NSF)
- Science and Technology Facilities Council (STFC) of the United Kingdom
- Max-Planck-Society (MPS)
- State of Niedersachsen/Germany
- Australian Research Council
- Italian Istituto Nazionale di Fisica Nucleare (INFN)
- French Centre National de la Recherche Scientifique (CNRS)
- Foundation for Fundamental Research on Matter
- Netherlands Organisation for Scientific Research
- EGO consortium
- STFC [ST/L000954/1, ST/J00166X/1, ST/N000072/1, ST/P000258/1, ST/K005014/1, Gravitational Waves, PPA/G/S/2002/00652, ST/N00003X/1, ST/M005844/1, ST/M000931/1, 1802894, ST/N005481/1, 1945971, ST/L000911/1, ST/K005014/2, ST/N005406/1, ST/R00045X/1, ST/N005406/2, 1653089, 1654298, ST/N005430/1, ST/K000845/1, ST/N005422/1, 2142081, ST/I006277/1, ST/H002006/1, 1802888, ST/N000633/1, ST/I006269/1] Funding Source: UKRI
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On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parametrization of the defining function p(rho) of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as R-1 = 10.8(-1.7)(+2.0) km for the heavier star and R-2 = 10.7(-1.5)(+2.1) km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than 1.97 M-circle dot as required from electromagnetic observations and employ the equation-of-state parametrization, we further constrain R-1 = 11.9(-1.4)(+1.4) km and R-2 = 11.9(-1.4)(+1.4) km at the 90% credible level. Finally, we obtain constraints on p(rho) at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5(-1.7)(+2.7) x 10(34) dyn cm(-2) at the 90% level.
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