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Title: Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities

Abstract

Here, we perform a systematic assessment of models for the equation of state (EOS) of dense matter in the context of recent neutron star mass and radius measurements to obtain a broad picture of the structure of neutron stars. We demonstrate that currently available neutron star mass and radius measurements provide strong constraints on moments of inertia, tidal deformabilities, and crust thicknesses. Moreover, a measurement of the moment of inertia of PSR J0737-3039A with a 10% error, without any other information from observations, will constrain the EOS over a range of densities to within 50% 60%. We find tidal deformabilities between 0.6 and 6 1036 g cm 2 s 2 (to 95% confidence) for M = 1.4 M , and any measurement which constrains this range will provide an important constraint on dense matter. The crustal fraction of the moment of inertia can be as large as 10% for M = 1.4 M permitting crusts to have a large enough moment of inertia reservoir to explain glitches in the Vela pulsar even with a large amount of superfluid entrainment. Finally, due to the uncertainty in the equation of state, there is at least a 40% variation in themore » thickness of the crust for a fixed mass and radius, which implies that future simulations of the cooling of a neutron star crust which has been heated by accretion will need to take this variation into account.« less

Authors:
 [1];  [2];  [3];  [4]
  1. Univ. of Washington, Seattle, WA (United States); Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  3. Texas A & M Univ., Commerce, TX (United States); Indiana Univ., Bloomington, IN (United States)
  4. Texas A & M Univ., Commerce, TX (United States)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1265810
Alternate Identifier(s):
OSTI ID: 1180490; OSTI ID: 1409749
Report Number(s):
LA-UR-14-21809
Journal ID: ISSN 0556-2813; PRVCAN; KB0301020; ERKBP05
Grant/Contract Number:  
AC05-00OR22725; FG02-00ER41132; AC02-05CH11231; AC52-06NA25396
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review. C, Nuclear Physics
Additional Journal Information:
Journal Volume: 91; Journal Issue: 1; Journal ID: ISSN 0556-2813
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
73 NUCLEAR PHYSICS AND RADIATION PHYSICS

Citation Formats

Steiner, A. W., Gandolfi, S., Fattoyev, F. J., and Newton, W. G. Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities. United States: N. p., 2015. Web. doi:10.1103/PhysRevC.91.015804.
Steiner, A. W., Gandolfi, S., Fattoyev, F. J., & Newton, W. G. Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities. United States. doi:10.1103/PhysRevC.91.015804.
Steiner, A. W., Gandolfi, S., Fattoyev, F. J., and Newton, W. G. Tue . "Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities". United States. doi:10.1103/PhysRevC.91.015804. https://www.osti.gov/servlets/purl/1265810.
@article{osti_1265810,
title = {Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities},
author = {Steiner, A. W. and Gandolfi, S. and Fattoyev, F. J. and Newton, W. G.},
abstractNote = {Here, we perform a systematic assessment of models for the equation of state (EOS) of dense matter in the context of recent neutron star mass and radius measurements to obtain a broad picture of the structure of neutron stars. We demonstrate that currently available neutron star mass and radius measurements provide strong constraints on moments of inertia, tidal deformabilities, and crust thicknesses. Moreover, a measurement of the moment of inertia of PSR J0737-3039A with a 10% error, without any other information from observations, will constrain the EOS over a range of densities to within 50% 60%. We find tidal deformabilities between 0.6 and 6 1036 g cm2 s2 (to 95% confidence) for M = 1.4 M⊙ , and any measurement which constrains this range will provide an important constraint on dense matter. The crustal fraction of the moment of inertia can be as large as 10% for M = 1.4 M⊙ permitting crusts to have a large enough moment of inertia reservoir to explain glitches in the Vela pulsar even with a large amount of superfluid entrainment. Finally, due to the uncertainty in the equation of state, there is at least a 40% variation in the thickness of the crust for a fixed mass and radius, which implies that future simulations of the cooling of a neutron star crust which has been heated by accretion will need to take this variation into account.},
doi = {10.1103/PhysRevC.91.015804},
journal = {Physical Review. C, Nuclear Physics},
number = 1,
volume = 91,
place = {United States},
year = {2015},
month = {1}
}

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