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Title: Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817

Abstract

In this study, we use gravitational-wave observations of the binary neutron star merger GW170817 to explore the tidal deformabilities and radii of neutron stars. We perform a Bayesian parameter estimation with the source location and distance informed by electromagnetic observations. We also assume that the two stars have the same equation of state; we demonstrate that, for stars with masses comparable to the component masses of GW170817, this is effectively implemented by assuming that the stars’ dimensionless tidal deformabilities are determined by the binary’s mass ratio q by Λ 12 = q 6. We investigate different choices of prior on the component masses of the neutron stars. We find that the tidal deformability and 90% credible interval is ˜Λ = 222$$+420\atop{-138}$$ for a uniform component mass prior, ˜Λ = 245$$+453\atop{-151}$$ for a component mass prior informed by radio observations of Galactic double neutron stars, and ˜Λ = 233$$+448\atop{-144}$$ for a component mass prior informed by radio pulsars. We find a robust measurement of the common areal radius of the neutron stars across all mass priors of 8.9 ≤ $$\hat{R}$$ ≤ 13.2 km , with a mean value of <$$\hat{R}$$> = 10.8 km . Finally, our results are the first measurement of tidal deformability with a physical constraint on the star’s equation of state and place the first lower bounds on the deformability and areal radii of neutron stars using gravitational waves.

Authors:
 [1];  [1];  [2];  [1];  [3]; ORCiD logo [4]
  1. Syracuse Univ., NY (United States)
  2. Stony Brook Univ., NY (United States)
  3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  4. Syracuse Univ., NY (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE; National Science Foundation (NSF)
OSTI Identifier:
1484643
Alternate Identifier(s):
OSTI ID: 1467957
Report Number(s):
LA-UR-18-23911
Journal ID: ISSN 0031-9007; PRLTAO
Grant/Contract Number:  
89233218CNA000001; FG02-87ER40317
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review Letters
Additional Journal Information:
Journal Volume: 121; Journal Issue: 9; Journal ID: ISSN 0031-9007
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

De, Soumi, Finstad, Daniel, Lattimer, James, Brown, Duncan A., Berger, Edo, and Biwer, Christopher Michael. Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817. United States: N. p., 2018. Web. doi:10.1103/PhysRevLett.121.091102.
De, Soumi, Finstad, Daniel, Lattimer, James, Brown, Duncan A., Berger, Edo, & Biwer, Christopher Michael. Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817. United States. doi:10.1103/PhysRevLett.121.091102.
De, Soumi, Finstad, Daniel, Lattimer, James, Brown, Duncan A., Berger, Edo, and Biwer, Christopher Michael. Wed . "Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817". United States. doi:10.1103/PhysRevLett.121.091102. https://www.osti.gov/servlets/purl/1484643.
@article{osti_1484643,
title = {Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817},
author = {De, Soumi and Finstad, Daniel and Lattimer, James and Brown, Duncan A. and Berger, Edo and Biwer, Christopher Michael},
abstractNote = {In this study, we use gravitational-wave observations of the binary neutron star merger GW170817 to explore the tidal deformabilities and radii of neutron stars. We perform a Bayesian parameter estimation with the source location and distance informed by electromagnetic observations. We also assume that the two stars have the same equation of state; we demonstrate that, for stars with masses comparable to the component masses of GW170817, this is effectively implemented by assuming that the stars’ dimensionless tidal deformabilities are determined by the binary’s mass ratio q by Λ1/Λ2 = q6. We investigate different choices of prior on the component masses of the neutron stars. We find that the tidal deformability and 90% credible interval is ˜Λ = 222$+420\atop{-138}$ for a uniform component mass prior, ˜Λ = 245$+453\atop{-151}$ for a component mass prior informed by radio observations of Galactic double neutron stars, and ˜Λ = 233$+448\atop{-144}$ for a component mass prior informed by radio pulsars. We find a robust measurement of the common areal radius of the neutron stars across all mass priors of 8.9 ≤ $\hat{R}$ ≤ 13.2 km , with a mean value of <$\hat{R}$> = 10.8 km . Finally, our results are the first measurement of tidal deformability with a physical constraint on the star’s equation of state and place the first lower bounds on the deformability and areal radii of neutron stars using gravitational waves.},
doi = {10.1103/PhysRevLett.121.091102},
journal = {Physical Review Letters},
number = 9,
volume = 121,
place = {United States},
year = {2018},
month = {8}
}

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Figures / Tables:

FIG. 1 FIG. 1: The tidal deformability Λ as a function of mass for physically realistic polytropes. A TOV integration with each EOS parameter set results in a series of values of Λ (m) that are shown as points colored by their radii R. Dashed curves are lower bounds to Λ formore » a given mass m which vary depending on the assumed lower limit to the neutron star maximum mass, mmax. All values of mmax produce the same upper bound.« less

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