Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations
Abstract
Here, the dense matter equation of state (EOS) determines neutron star (NS) structure but can be calculated reliably only up to one to two times the nuclear saturation density, using accurate many-body methods that employ nuclear interactions from chiral effective field theory constrained by scattering data. In this work, we use physically motivated ansatzes for the speed of sound c S at high density to extend microscopic calculations of neutron-rich matter to the highest densities encountered in stable NS cores. We show how existing and expected astrophysical constraints on NS masses and radii from X-ray observations can constrain the speed of sound in the NS core. We confirm earlier expectations that c S is likely to violate the conformal limit of $${c}_{S}^{2}\leqslant {c}^{2}/3$$, possibly reaching values closer to the speed of light c at a few times the nuclear saturation density, independent of the nuclear Hamiltonian. If QCD obeys the conformal limit, we conclude that the rapid increase of c S required to accommodate a 2 M ⊙ NS suggests a form of strongly interacting matter where a description in terms of nucleons will be unwieldy, even between one and two times the nuclear saturation density. For typical NSs with masses in the range of 1.2–1.4 M ⊙, we find radii between 10 and 14 km, and the smallest possible radius of a 1.4 M ⊙ NS consistent with constraints from nuclear physics and observations is 8.4 km. We also discuss how future observations could constrain the EOS and guide theoretical developments in nuclear physics.
- Authors:
-
- Univ. of Washington, Seattle, WA (United States); Michigan State Univ., East Lansing, MI (United States)
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Publication Date:
- Research Org.:
- Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE Laboratory Directed Research and Development (LDRD) Program
- OSTI Identifier:
- 1481144
- Report Number(s):
- LA-UR-17-31455
Journal ID: ISSN 1538-4357
- Grant/Contract Number:
- AC52-06NA25396
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 860; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy and Astrophysics; dense matter; equation of state; stars: neutron
Citation Formats
Tews, I., Carlson, Joseph Allen, Gandolfi, Stefano, and Reddy, S. Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations. United States: N. p., 2018.
Web. doi:10.3847/1538-4357/aac267.
Tews, I., Carlson, Joseph Allen, Gandolfi, Stefano, & Reddy, S. Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations. United States. https://doi.org/10.3847/1538-4357/aac267
Tews, I., Carlson, Joseph Allen, Gandolfi, Stefano, and Reddy, S. Wed .
"Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations". United States. https://doi.org/10.3847/1538-4357/aac267. https://www.osti.gov/servlets/purl/1481144.
@article{osti_1481144,
title = {Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations},
author = {Tews, I. and Carlson, Joseph Allen and Gandolfi, Stefano and Reddy, S.},
abstractNote = {Here, the dense matter equation of state (EOS) determines neutron star (NS) structure but can be calculated reliably only up to one to two times the nuclear saturation density, using accurate many-body methods that employ nuclear interactions from chiral effective field theory constrained by scattering data. In this work, we use physically motivated ansatzes for the speed of sound c S at high density to extend microscopic calculations of neutron-rich matter to the highest densities encountered in stable NS cores. We show how existing and expected astrophysical constraints on NS masses and radii from X-ray observations can constrain the speed of sound in the NS core. We confirm earlier expectations that c S is likely to violate the conformal limit of ${c}_{S}^{2}\leqslant {c}^{2}/3$, possibly reaching values closer to the speed of light c at a few times the nuclear saturation density, independent of the nuclear Hamiltonian. If QCD obeys the conformal limit, we conclude that the rapid increase of c S required to accommodate a 2 M ⊙ NS suggests a form of strongly interacting matter where a description in terms of nucleons will be unwieldy, even between one and two times the nuclear saturation density. For typical NSs with masses in the range of 1.2–1.4 M ⊙, we find radii between 10 and 14 km, and the smallest possible radius of a 1.4 M ⊙ NS consistent with constraints from nuclear physics and observations is 8.4 km. We also discuss how future observations could constrain the EOS and guide theoretical developments in nuclear physics.},
doi = {10.3847/1538-4357/aac267},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 860,
place = {United States},
year = {Wed Jun 20 00:00:00 EDT 2018},
month = {Wed Jun 20 00:00:00 EDT 2018}
}
Web of Science
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From the microscopic to the macroscopic world: from nucleons to neutron stars
text, January 2019
- Gandolfi, S.; Lippuner, J.; Steiner, A. W.
- arXiv
Signatures for quark matter from multi-messenger observations
text, January 2019
- Alford, Mark G.; Han, Sophia; Schwenzer, Kai
- arXiv
New constraints on the nuclear equation of state from the thermal emission of neutron stars in quiescent low-mass X-ray binaries
text, January 2019
- d'Etivaux, N. Baillot; Guillot, S.; Margueron, J.
- arXiv
Treating quarks within neutron stars
text, January 2019
- Han, Sophia; Mamun, M. A. A.; Lalit, S.
- arXiv
Neutron Star Matter as a Relativistic Fermi Liquid
text, January 2019
- Friman, Bengt; Weise, Wolfram
- arXiv
A NICER view of PSR J0030+0451: Implications for the dense matter equation of state
text, January 2019
- Raaijmakers, G.; Riley, T. E.; Watts, A. L.
- arXiv
PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
text, January 2019
- Miller, M. C.; Lamb, F. K.; Dittmann, A. J.
- arXiv
Local nucleon-nucleon and three-nucleon interactions within chiral effective field theory
text, January 2020
- Piarulli, Maria; Tews, Ingo
- arXiv
Extensive studies of the neutron star equation of state from the deep learning inference with the observational data augmentation
journal, March 2021
- Fujimoto, Yuki; Fukushima, Kenji; Murase, Koichi
- Journal of High Energy Physics, Vol. 2021, Issue 3
Speed of sound constraints on maximally rotating neutron stars
journal, February 2020
- Margaritis, Ch.; Koliogiannis, P. S.; Moustakidis, Ch. C.
- Physical Review D, Vol. 101, Issue 4
Local Nucleon-Nucleon and Three-Nucleon Interactions Within Chiral Effective Field Theory
journal, January 2020
- Piarulli, Maria; Tews, Ingo
- Frontiers in Physics, Vol. 7
Atomic Nuclei From Quantum Monte Carlo Calculations With Chiral EFT Interactions
journal, April 2020
- Gandolfi, Stefano; Lonardoni, Diego; Lovato, Alessandro
- Frontiers in Physics, Vol. 8
Local chiral EFT potentials in nuclei and neutron matter: results and issues
preprint, January 2019
- Lonardoni, Diego; Tews, Ingo
- arXiv
Neutron star equation of state: QMF modeling and applications
text, January 2020
- Li, A.; Zhu, Z. -Y.; Zhou, E. -P.
- arXiv
Relativistic fluid dynamics: physics for many different scales
text, January 2020
- Andersson, N.; Comer, G. L. C.
- arXiv
NMMA: A nuclear-physics and multi-messenger astrophysics framework to analyze binary neutron star mergers
preprint, January 2022
- Pang, Peter T. H.; Dietrich, Tim; Coughlin, Michael W.
- arXiv