Testing the Formation Scenarios of Binary Neutron Star Systems with Measurements of the Neutron Star Moment of Inertia
Abstract
Two low-mass (M < 1.4 M ⊙) neutron stars, J0737-3039B and the companion to J1756-2251, show strong evidence of being formed in an ultra-stripped supernova explosion (US-SN) with a ONeMg or Fe progenitor. In this paper, using systematically generated sets of equations of state we map out the relationship between the moment of inertia of J0737-3039A, a candidate for a moment of inertia measurement within a decade, and the binding energy of the two low-mass neutron stars. This relationship, similar to the I-Love-Q relations, is more robust than a previously explored correlation between the binding energy and the slope of the nuclear symmetry energy L. We find that, if either J0737-3039B or the J1756-2251 companion were formed in a US-SN, no more than 0.06 M ⊙ could have been lost from the progenitor core. Furthermore, a measurement of the moment of inertia of J0737-3039A to within 10% accuracy can discriminate between formation scenarios and, given current constraints on the predicted core mass loss, potentially rule them out. Advanced LIGO can potentially measure the neutron star tidal polarizability to equivalent accuracy which, using the I-Love-Q relations, would obtain similar constraints on the formation scenarios. Such information would help constrain important aspectsmore »
- Authors:
-
[2];
- Texas A & M Univ., Commerce, TX (United States). Dept. of Physics and Astronomy
- Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
- Univ. of Virginia, Charlottesville, VA (United States). Dept. of Physics
- Publication Date:
- Research Org.:
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States); Univ. of Virginia, Charlottesville, VA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF)
- OSTI Identifier:
- 1460183
- Grant/Contract Number:
- AC05-00OR22725; PHY 15-54876; PHY-1305682
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 856; Journal Issue: 1; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; binaries; close; dense matter; equation of state; pulsars; star evolution; neutron stars
Citation Formats
Newton, William G., Steiner, Andrew W., and Yagi, Kent. Testing the Formation Scenarios of Binary Neutron Star Systems with Measurements of the Neutron Star Moment of Inertia. United States: N. p., 2018.
Web. doi:10.3847/1538-4357/aaafd1.
Newton, William G., Steiner, Andrew W., & Yagi, Kent. Testing the Formation Scenarios of Binary Neutron Star Systems with Measurements of the Neutron Star Moment of Inertia. United States. https://doi.org/10.3847/1538-4357/aaafd1
Newton, William G., Steiner, Andrew W., and Yagi, Kent. Wed .
"Testing the Formation Scenarios of Binary Neutron Star Systems with Measurements of the Neutron Star Moment of Inertia". United States. https://doi.org/10.3847/1538-4357/aaafd1. https://www.osti.gov/servlets/purl/1460183.
@article{osti_1460183,
title = {Testing the Formation Scenarios of Binary Neutron Star Systems with Measurements of the Neutron Star Moment of Inertia},
author = {Newton, William G. and Steiner, Andrew W. and Yagi, Kent},
abstractNote = {Two low-mass (M < 1.4 M ⊙) neutron stars, J0737-3039B and the companion to J1756-2251, show strong evidence of being formed in an ultra-stripped supernova explosion (US-SN) with a ONeMg or Fe progenitor. In this paper, using systematically generated sets of equations of state we map out the relationship between the moment of inertia of J0737-3039A, a candidate for a moment of inertia measurement within a decade, and the binding energy of the two low-mass neutron stars. This relationship, similar to the I-Love-Q relations, is more robust than a previously explored correlation between the binding energy and the slope of the nuclear symmetry energy L. We find that, if either J0737-3039B or the J1756-2251 companion were formed in a US-SN, no more than 0.06 M ⊙ could have been lost from the progenitor core. Furthermore, a measurement of the moment of inertia of J0737-3039A to within 10% accuracy can discriminate between formation scenarios and, given current constraints on the predicted core mass loss, potentially rule them out. Advanced LIGO can potentially measure the neutron star tidal polarizability to equivalent accuracy which, using the I-Love-Q relations, would obtain similar constraints on the formation scenarios. Such information would help constrain important aspects of binary evolution used for population synthesis predictions of the rate of binary neutron star mergers and resulting electromagnetic and gravitational wave signals. Finally, further progress needs to be made in modeling the core-collapse process that leads to low-mass neutron stars, particularly in making robust predictions for the mass loss from the progenitor core.},
doi = {10.3847/1538-4357/aaafd1},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 856,
place = {United States},
year = {Wed Mar 21 00:00:00 EDT 2018},
month = {Wed Mar 21 00:00:00 EDT 2018}
}
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Neutrino-driven explosions of ultra-stripped type Ic supernovae generating binary neutron stars
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Formation of Double Neutron Star systems as implied by observations
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Long Term Study of the Double Pulsar J0737-3039 with XMM-Newton: pulsar timing
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Do electron-capture supernovae make neutron stars? First multidimensional hydrodynamic simulations of the oxygen deflagration
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Masses, Radii, and Equation of State of Neutron Stars
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Approximate Universal Relations for Neutron Stars and Quark Stars
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GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
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The Role of Helium Stars in the Formation of Double Neutron Stars
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