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Phys Rev Lett. 2018 Oct 19;121(16):161101. doi: 10.1103/PhysRevLett.121.161101.

GW170817: Measurements of Neutron Star Radii and Equation of State.

Abbott BP, Abbott R, Abbott TD, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari RX, Adya VB, Affeldt C, Agarwal B, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen B, Allen G, Allocca A, Aloy MA, Altin PA, Amato A, Ananyeva A, Anderson SB, Anderson WG, Angelova SV, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Arun KG, Ascenzi S, Ashton G, Ast M, Aston SM, Astone P, Atallah DV, Aubin F, Aufmuth P, Aulbert C, AultONeal K, Austin C, Avila-Alvarez A, Babak S, Bacon P, Badaracco F, Bader MKM, Bae S, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Banagiri S, Barayoga JC, Barclay SE, Barish BC, Barker D, Barkett K, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Batch JC, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Beer C, Bejger M, Belahcene I, Bell AS, Beniwal D, Bensch M, Berger BK, Bergmann G, Bernuzzi S, Bero JJ, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bilenko IA, Bilgili SA, Billingsley G, Billman CR, Birch J, Birney R, Birnholtz O, Biscans S, Biscoveanu S, Bisht A, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bloemen S, Bock O, Bode N, Boer M, Boetzel Y, Bogaert G, Bohe A, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Booth CD, Bork R, Boschi V, Bose S, Bossie K, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Briant T, Brighenti F, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DD, Brunett S, Buchanan CC, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Calderón Bustillo J, Callister TA, Calloni E, Camp JB, Canepa M, Canizares P, Cannon KC, Cao H, Cao J, Capano CD, Capocasa E, Carbognani F, Caride S, Carney MF, Carullo G, Casanueva Diaz J, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cepeda CB, Cerdá-Durán P, Cerretani G, 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B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Wellmann F, Wen L, Wessel EK, Weßels P, Westerweck J, Wette K, Whelan JT, Whiting BF, Whittle C, Wilken D, Williams D, Williams RD, Williamson AR, Willis JL, Willke B, Wimmer MH, Winkler W, Wipf CC, Wittel H, Woan G, Woehler J, Wofford JK, Wong WK, Worden J, Wright JL, Wu DS, Wysocki DM, Xiao S, Yam W, Yamamoto H, Yancey CC, Yang L, Yap MJ, Yazback M, Yu H, Yu H, Yvert M, Zadrożny A, Zanolin M, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang M, Zhang T, Zhang YH, Zhao C, Zhou M, Zhou Z, Zhu SJ, Zhu XJ, Zimmerman AB, Zlochower Y, Zucker ME, Zweizig J; LIGO Scientific Collaboration and the Virgo Collaboration.

Abstract

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(ρ) 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_{⊙} 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(ρ) at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5_{-1.7}^{+2.7}×10^{34}  dyn cm^{-2} at the 90% level.

PMID:
30387654
DOI:
10.1103/PhysRevLett.121.161101
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