Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations

Tews, I.; Carlson, Joseph Allen; Gandolfi, Stefano; Reddy, S.

doi:10.3847/1538-4357/aac267

Title: Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations

Journal Article · Wed Jun 20 00:00:00 EDT 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aac267· OSTI ID:1481144

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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)

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.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE Laboratory Directed Research and Development (LDRD) Program

Grant/Contract Number:: AC52-06NA25396

OSTI ID:: 1481144

Report Number(s):: LA-UR-17-31455

Journal Information:: The Astrophysical Journal (Online), Vol. 860, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 175 works

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Sound velocity and tidal deformability in compact stars Ma, Yong-Liang; Rho, Mannque arXiv https://doi.org/10.48550/arxiv.1811.07071	text	January 2018
Constraining twin stars with GW170817 Montana, Gloria; Tolos, Laura; Hanauske, Matthias arXiv https://doi.org/10.48550/arxiv.1811.10929	text	January 2018
Quarkyonic Matter and Neutron Stars McLerran, Larry; Reddy, Sanjay arXiv https://doi.org/10.48550/arxiv.1811.12503	text	January 2018
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