Constraints on a phenomenologically parametrized neutron-star equation of state

By J. Read, B. Lackey, B. Owen, J. Friedman. 2008

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We introduce a parametrized high-density equation of state (EOS) in order to systematize the study of constraints placed by astrophysical observations on the nature of neutron-star matter. To obtain useful constraints, the number of parameters must be smaller than the number of EOS-related neutron-star properties measured, but large enough to accurately approximate the large set of candidate EOSs. We find that a parametrized EOS based on piecewise polytropes with 3 free parameters matches, to about 4% rms error, an extensive set of candidate EOSs at densities below the central density of $1.4{M}_{\ensuremath{\bigodot}}$ stars. Adding observations of more massive stars constrains the higher-density part of the EOS and requires an additional parameter. We obtain constraints on the allowed parameter space set by causality and by present and near-future astronomical observations with the least model dependence. Stringent constraints on the EOS parameter space are associated with the future measurement of the moment of inertia of PSR J0737-3039A combined with the maximum known neutron-star mass. We also present in an appendix a more efficient algorithm than has previously been used for finding points of marginal stability and the maximum angular velocity of stable stars.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/eef4e80b5e90cbefaab4318f1afdd8ab134054a3

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Citations in the corpus

GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, unknown): “4chirpL = L = ˜ ˜ ( ) ( ) We consider a set of 12 EOSs: the four used in the simulations and the other eight from Read et al. (2009).”
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, methodology): “Measurements of NS masses and radii together can put strong constraints on the EoS (Read et al. 2009; Özel & Psaltis 2009; Özel et al. 2010; Steiner et al. 2010; Guillot et al. 2013; Steiner et al. 2013a,b; Özel et al. 2016).”
A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation (2019, methodology): “Given a suitable model for the EOS (see, e.g., Read et al. 2009; Raithel et al. 2016; Tews et al. 2018a; Lindblom 2018) there are two approaches to EOS inference: one is to jointly infer the EOS parameters (and central densities) directly from the data (e.g., pulse-profile data); the other is to…”
Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, background): “In one of the first quantitative studies exploring EOS effects on the waveform from the coalescence of two neutron stars, Read et al. (2009b) showed that a realistic waveform would deviate significantly from a point-particle waveform and that this could be observed with Advanced LIGO.”
Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, methodology): “The multi-parameters polytropic EOSs, see, e.g., refs (Topper 1964; Butterworth 1976; Read et al. 2009) are widely used in modeling the core EOS of neutron stars at suprasaturation densities.”
THE EQUATION OF STATE FROM OBSERVED MASSES AND RADII OF NEUTRON STARS (2010, methodology): “Read et al. (2009) showed that piecewise polytropes with relatively few parameters could eff ctively describe more sophisticated models for a high-density EOS, but confined attention to constraints stemming from observations limiting the neutron star maximum mass and maximum spin rate.”
A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars (2014, background): “…the EoS to yield a third family and/or the twin phenomenon, the following two conditions should be fulfilled (for details, see Haensel et al. 2007; Read et al. 2009; Zdunik & Haensel 2013; Alford et al. 2013): (1) The latent heat of the phase transition should fulfil a constraint Δε > Δεmin…”