Neutron star radii and crusts: Uncertainties and unified equations of state
By M. Fortin, Constança Providência, Adriana Raduta, F. Gulminelli, J. Zdunik, P. Haensel, Michal Bejger. 2016
201 citations recorded by the source corpus.
The uncertainties in neutron star radii and crust properties due to our limited knowledge of the equation of state are quantitatively analyzed. We first demonstrate the importance of a unified microscopic description for the different baryonic densities of the star. If the pressure functional is obtained matching a crust and a core equation of state based on models with different properties at nuclear matter saturation, the uncertainties can be as large as $\ensuremath{\sim}30$ % for the crust thickness and 4% for the radius. Necessary conditions for causal and thermodynamically consistent matchings between the core and the crust are formulated and their consequences examined. A large set of unified equations of state for purely nucleonic matter is obtained based on twenty-four Skyrme interactions and nine relativistic mean-field nuclear parametrizations. In addition, for relativistic models fifteen equations of state including a transition to hyperonic matter at high density are presented. All these equations of state have in common the property of describing a $2{M}_{\ensuremath{\bigodot}}$ star and of being causal within stable neutron stars. Spans of $\ensuremath{\sim}3$ and $\ensuremath{\sim}4$ km are obtained for the radius of, respectively, $1.0{M}_{\ensuremath{\bigodot}}$ and $2.0{M}_{\ensuremath{\bigodot}}$ stars. Applying a set of nine further constraints from experiment and ab initio calculations the uncertainty is reduced to $\ensuremath{\sim}1$ and 2 km, respectively. These residual uncertainties reflect lack of constraints at large densities and insufficient information on the density dependence of the equation of state near the nuclear matter saturation point. The most important parameter to be constrained is shown to be the symmetry energy slope $L$. Indeed, this parameter exhibits a linear correlation with the stellar radius, which is particularly clear for small mass stars around $1.0{M}_{\ensuremath{\bigodot}}$. The other equation-of-state parameters do not show clear correlations with the radius, within the present uncertainties. Potential constraints on $L$, the neutron star radius, and the equation of state from observations of thermal states of neutron stars are also discussed. The unified equations of state are made available in the Supplemental Materials and via the CompOSE database.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/217be271bdb88cd056775ec966c04e1ceb4ce299
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Citations in the corpus
- Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, methodology): “[107] within the Skyrme Hartree-Fock and the RMF models for the core and the Thomas-Fermi model for the crust using the same interactions.”
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. I. Role of symmetry energy (2018, result): “This reflects the correlation between L and RNS known from previous studies (e.g., Fortin et al. 2016; Margueron et al. 2018).”
- Superfluidity in nuclear systems and neutron stars (2018, background): “Because this involves input for the composition of matter and self-energy effects, the results depend on the chosen DFs, which are labeled as DDME2 (Fortin et al., 2016), GM1A (Gusakov et al., 2014), and SWL (Spinella, 2017).”