EQUATION OF STATE AND NEUTRON STAR PROPERTIES CONSTRAINED BY NUCLEAR PHYSICS AND OBSERVATION

By K. Hebeler, J. Lattimer, C. Pethick, A. Schwenk. 2013

474 citations recorded by the source corpus.

Microscopic calculations of neutron matter based on nuclear interactions derived from chiral effective field theory, combined with the recent observation of a 1.97 ± 0.04 M☉ neutron star, constrain the equation of state of neutron-rich matter at sub- and supranuclear densities. We discuss in detail the allowed equations of state and the impact of our results on the structure of neutron stars, the crust-core transition density, and the nuclear symmetry energy. In particular, we show that the predicted range for neutron star radii is robust. For use in astrophysical simulations, we provide detailed numerical tables for a representative set of equations of state consistent with these constraints.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3bd816146f726a28d894d940e01248e10d00b0ec

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Citations in the corpus

Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “For the second branch, using the blend of soft, middle and stiff EOS of [220], stable configurations are found whose masses, for d < 0, generally grow with b and are basically unconstrained from above, even to a greater extent than in the quadratic f (R) case considered also in [97], with a signific”
Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, background): “The parameter α;1/137 is the fine-structure constant, and η is determined by densitygradient terms in the nuclear Hamiltonian and can be approximated by D 1 4 np nn np nn 2h m m m m= - +[ ( ) ], where D=4Q/3;81MeV fm5 (Hebeler et al. 2013).”
From hadrons to quarks in neutron stars: a review (2017, background): “For example, in the early MIT bag model, B ' (145-155) MeV4 ' (60-80) MeV/fm3.”
NEUTRON STAR MASSES AND RADII FROM QUIESCENT LOW-MASS X-RAY BINARIES (2013, background): “…nuclear experimental (Newton et al. 2011; Tsang et al. 2012; Lattimer & Lim 2013) and theoretical neutron matter studies (Steiner & Gandolfi 2012; Hebeler et al. 2013), about 10.7–13.1 km and 10 – 13.7 km, respectively, with all confidence regions being 90% However, the uncertainties in NH…”
Constraining the mass and radius of neutron stars in globular clusters (2017, background): “Hebeler et al. (2013) and Steiner et al. (2016) have shown that neutron star radii are between 11 and 13 km, assuming that chiral effective theory approaches to neutron matter can be employed above the nuclear saturation density.”
Unified equation of state for neutron stars on a microscopic basis (2015, background): “…values for Esym(n0) and L lie within the recent constraints derived from the analysis of different astrophysical observations (Newton et al. 2013; Steiner et al. 2010; Lattimer & Lim 2013; Hebeler et al. 2013) and nuclear experiments (Chen et al. 2010; Tsang et al. 2012; Viñas et al. 2014).”
Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “On the other hand, the detection or non-detection of the signatures we predict would be a critical test of NS equations of state (Hebeler et al. 2013).”