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A Parametrized Equation of State for Neutron Star Matter with Continuous Sound Speed

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arxiv 2008.03342 v2 pith:AEOZN3ZI submitted 2020-08-07 astro-ph.HE gr-qc

Michael F. O'Boyle , Charalampos Markakis , Nikolaos Stergioulas , Jocelyn S. Read This is my paper · ORCID
classification astro-ph.HEgr-qc
keywords piecewisegeneralizedpolytropesstateastrophysicalequationneutronobservables
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We present a generalized piecewise polytropic parameterization for the neutron-star equation of state using an ansatz that imposes continuity in not only pressure and energy density, but also in the speed of sound. The universe of candidate equations of state is shown to admit preferred dividing densities, determined by minimizing an error norm consisting of integral astrophysical observables. Generalized piecewise polytropes accurately reproduce astrophysical observables, such as mass, radius, tidal deformability and mode frequencies, as well as thermodynamic quantities, such as the adiabatic index. This makes the new EOS useful for Bayesian parameter estimation from gravitational waveforms. Moreover, since they are differentiable, generalized piecewise polytropes can improve pointwise convergence in numerical relativity simulations of neutron stars. Existing implementations of piecewise polytropes can easily accommodate this generalization.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Systematic study of the morphology and length of slow stable hybrid star branches

    astro-ph.HE 2026-06 unverdicted novelty 7.0 of 10

    Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.

  2. Combining simulation-based inference and universal relations for precise and accurate neutron star science

    gr-qc 2026-01 conditional novelty 6.0 of 10

    A machine-learning simulator trained on 1,491 simulated equations of state discovers a neutron-star radius relation R(M,f,p1), predicting radii to tens of meters with calibrated error bars.

  3. Rotating neutron stars: anisotropy model comparison

    astro-ph.HE 2025-04 conditional novelty 5.0 of 10

    Anisotropic pressure can raise the maximum stable neutron-star mass by 50-60 percent in the covariant model, and normalized moment of inertia and binding energy follow nearly model-independent fits.

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