Neutron star radii, universal relations, and the role of prior distributions
We investigate constraints on neutron star structure arising from the assumptions that neutron stars have crusts, that recent calculations of pure neutron matter limit the equation of state of neutron star matter near the nuclear saturation density, that the highdensity equation of state is limited by causality and the largest highaccuracy neutron star mass measurement, and that general relativity is the correct theory of gravity. We explore the role of prior assumptions by considering two classes of equation of state models. In a first, the intermediate and highdensity behavior of the equation of state is parameterized by piecewise polytropes. In the second class, the highdensity behavior of the equation of state is parameterized by piecewise continuous line segments. The smallest density at which highdensity matter appears is varied in order to allow for strong phase transitions above the nuclear saturation density. We critically examine correlations among the pressure of matter, radii, maximum masses, the binding energy, the moment of inertia, and the tidal deformability, paying special attention to the sensitivity of these correlations to prior assumptions about the equation of state. It is possible to constrain the radii of 1.4 solar mass neutron stars to be larger than 10 km,more »
 Authors:

^{[1]};
^{[2]};
^{[3]}
 Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
 Stony Brook Univ., Stony Brook, NY (United States)
 Michigan State Univ., East Lansing, MI (United States)
 Publication Date:
 Grant/Contract Number:
 AC0500OR22725
 Type:
 Accepted Manuscript
 Journal Name:
 European Physical Journal. A
 Additional Journal Information:
 Journal Volume: 52; Journal Issue: 2; Journal ID: ISSN 14346001
 Publisher:
 Springer
 Research Org:
 Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States). Joint Institute for Computational Sciences (JICS)
 Sponsoring Org:
 USDOE Office of Science (SC)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTRONOMY AND ASTROPHYSICS; neutron stars; nuclear matter aspects of neutron stars; Xray binaries; nuclear matter
 OSTI Identifier:
 1267044
Steiner, Andrew W., Lattimer, James M., and Brown, Edward F.. Neutron star radii, universal relations, and the role of prior distributions. United States: N. p.,
Web. doi:10.1140/epja/i2016160181.
Steiner, Andrew W., Lattimer, James M., & Brown, Edward F.. Neutron star radii, universal relations, and the role of prior distributions. United States. doi:10.1140/epja/i2016160181.
Steiner, Andrew W., Lattimer, James M., and Brown, Edward F.. 2016.
"Neutron star radii, universal relations, and the role of prior distributions". United States.
doi:10.1140/epja/i2016160181. https://www.osti.gov/servlets/purl/1267044.
@article{osti_1267044,
title = {Neutron star radii, universal relations, and the role of prior distributions},
author = {Steiner, Andrew W. and Lattimer, James M. and Brown, Edward F.},
abstractNote = {We investigate constraints on neutron star structure arising from the assumptions that neutron stars have crusts, that recent calculations of pure neutron matter limit the equation of state of neutron star matter near the nuclear saturation density, that the highdensity equation of state is limited by causality and the largest highaccuracy neutron star mass measurement, and that general relativity is the correct theory of gravity. We explore the role of prior assumptions by considering two classes of equation of state models. In a first, the intermediate and highdensity behavior of the equation of state is parameterized by piecewise polytropes. In the second class, the highdensity behavior of the equation of state is parameterized by piecewise continuous line segments. The smallest density at which highdensity matter appears is varied in order to allow for strong phase transitions above the nuclear saturation density. We critically examine correlations among the pressure of matter, radii, maximum masses, the binding energy, the moment of inertia, and the tidal deformability, paying special attention to the sensitivity of these correlations to prior assumptions about the equation of state. It is possible to constrain the radii of 1.4 solar mass neutron stars to be larger than 10 km, even without consideration of additional astrophysical observations, for example, those from photospheric radius expansion bursts or quiescent lowmass Xray binaries. We are able to improve the accuracy of known correlations between the moment of inertia and compactness as well as the binding energy and compactness. Furthermore, we also demonstrate the existence of a correlation between the neutron star binding energy and the moment of inertia.},
doi = {10.1140/epja/i2016160181},
journal = {European Physical Journal. A},
number = 2,
volume = 52,
place = {United States},
year = {2016},
month = {2}
}