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Title: Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory

Abstract

The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints on neutron-star radii by combining multimessenger observations of the binary neutron-star merger GW170817 with nuclear theory that best accounts for density-dependent uncertainties in the equation of state. We construct equations of state constrained by chiral effective field theory and marginalize over these using the gravitational-wave observations. Combining this with the electromagnetic observations of the merger remnant that imply the presence of a short-lived hypermassive neutron star, we find that the radius of a 1.4 M⊙ neutron star is $$R_{1.4M_⊙} = 11.0^{+0.9}_{-0.6} km$$ (90% credible interval). Finally, using this constraint, we show that neutron stars are unlikely to be disrupted in neutron star–black hole mergers; subsequently, such events will not produce observable electromagnetic emission.

Authors:
ORCiD logo [1]; ORCiD logo [2];  [1];  [3];  [4];  [1]; ORCiD logo [4];  [1];  [5]
  1. Max Planck Inst. fur Gravitationphysik, Hannover (Germany); Leibniz Univ., Hannover (Germany)
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  3. Univ. of California, Berkeley, CA (United States); Univ. of California, Santa Barbara, CA (United States)
  4. Univ. of California, Santa Barbara, CA (United States); Syracuse Univ., NY (United States)
  5. Univ. of Washington, Seattle, WA (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program; USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF); National Aeronautic and Space Administration (NASA)
OSTI Identifier:
1614838
Report Number(s):
LA-UR-19-28442
Journal ID: ISSN 2397-3366
Grant/Contract Number:  
89233218CNA000001; PHY-1430152; PHY-1707954; FG02-00ER41132; HST-HF2-51412.001; NAS5-26555; AC02-06NA25396; PHY-1748958
Resource Type:
Accepted Manuscript
Journal Name:
Nature Astronomy
Additional Journal Information:
Journal Volume: 4; Journal ID: ISSN 2397-3366
Publisher:
Springer Nature
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; atomic; nuclear and particle physics; compact astrophysical objects; general relativity and gravity; nuclear astrophysics

Citation Formats

Capano, Collin D., Tews, Ingo, Brown, Stephanie M., Margalit, Ben, De, Soumi, Kumar, Sumit, Brown, Duncan A., Krishnan, Badri, and Reddy, Sanjay. Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory. United States: N. p., 2020. Web. doi:10.1038/s41550-020-1014-6.
Capano, Collin D., Tews, Ingo, Brown, Stephanie M., Margalit, Ben, De, Soumi, Kumar, Sumit, Brown, Duncan A., Krishnan, Badri, & Reddy, Sanjay. Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory. United States. doi:https://doi.org/10.1038/s41550-020-1014-6
Capano, Collin D., Tews, Ingo, Brown, Stephanie M., Margalit, Ben, De, Soumi, Kumar, Sumit, Brown, Duncan A., Krishnan, Badri, and Reddy, Sanjay. Mon . "Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory". United States. doi:https://doi.org/10.1038/s41550-020-1014-6. https://www.osti.gov/servlets/purl/1614838.
@article{osti_1614838,
title = {Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory},
author = {Capano, Collin D. and Tews, Ingo and Brown, Stephanie M. and Margalit, Ben and De, Soumi and Kumar, Sumit and Brown, Duncan A. and Krishnan, Badri and Reddy, Sanjay},
abstractNote = {The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints on neutron-star radii by combining multimessenger observations of the binary neutron-star merger GW170817 with nuclear theory that best accounts for density-dependent uncertainties in the equation of state. We construct equations of state constrained by chiral effective field theory and marginalize over these using the gravitational-wave observations. Combining this with the electromagnetic observations of the merger remnant that imply the presence of a short-lived hypermassive neutron star, we find that the radius of a 1.4 M⊙ neutron star is $R_{1.4M_⊙} = 11.0^{+0.9}_{-0.6} km$ (90% credible interval). Finally, using this constraint, we show that neutron stars are unlikely to be disrupted in neutron star–black hole mergers; subsequently, such events will not produce observable electromagnetic emission.},
doi = {10.1038/s41550-020-1014-6},
journal = {Nature Astronomy},
number = ,
volume = 4,
place = {United States},
year = {2020},
month = {3}
}

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Cited by: 19 works
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