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

By I. Tews, J. Carlson, Stefano Gandolfi, S. Reddy. Astrophysical Journal, 2018

367 citations recorded by the source corpus.

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 cS 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 cS is likely to violate the conformal limit of , 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 cS 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3e833ad602096dcd515a7f070451aa8bc3b32793

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Citations in the corpus

Dark halos around neutron stars and gravitational waves (2018, neutral): “4 M NS is in the range 10 − 13 km [43, 45, 46].”
On the Sound Speed in Neutron Stars (2022, background): “This behavior confirms on rather general grounds the tension between c 1 3s,max 2 < and the observation of stars with M 2Me, already been pointed out (see, e.g., Alford et al. 2015; Bedaque & Steiner 2015; Tews et al. 2018).”
A NICER View of PSR J0030+0451: Implications for the Dense Matter Equation of State (2019, methodology): “Following the methods described in Greif et al. (2019), we model the interior of PSRJ0030+0451 using two distinct EoS parameterizations: the piecewise-polytropic (PP) model from Hebeler et al. (2013) and a speed of sound (CS) model introduced in Greif et al. (2019)—see also Tews et al. (2018a).”
Science case for the Einstein telescope (2019, background): “However, despite the proximity of GW170817, the inferred constraints on the equation of state of NS matter [37] are too weak to discriminate between realistic models, nor do they offer new insights about phase transitions [38–40].”
Equation of state sensitivities when inferring neutron star and dense matter properties (2018, methodology): “(2) The form of our CS parametrization is very similar to the one used by Tews et al. (2018b).”