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Neutron Stars and the Nuclear Equation of State

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arxiv 2105.03747 v1 pith:734BNQK5 submitted 2021-05-08 nucl-th astro-ph.HE

G. F. Burgio , I. Vidana , H.-J. Schulze , J.-B. Wei (INFN Sezione di Catania) This is my paper · ORCID
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We review the current status and recent progress of microscopic many-body approaches and phenomenological models, which are employed to construct the equation of state of neutron stars. The equation of state is relevant for the description of their structure and dynamical properties, and it rules also the dynamics of core-collapse supernovae and binary neutron star mergers. We describe neutron star matter assuming that the main degrees of freedom are nucleons and hyperons, disregarding the appearance of quark matter. We compare the theoretical predictions of the different equation-of-state models with the currently available data coming from both terrestrial laboratory experiments and recent astrophysical observations. We also analyse the importance of the nuclear strong interaction and equation of state for the cooling properties of neutron stars. We discuss the main open challenges in the description of the equation of state, mainly focusing on the limits of the different many-body techniques, the so-called "hyperon puzzle," and the dependence of the direct URCA processes on the equation of state.

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Cited by 11 Pith papers

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

  1. Holographic Soliton Crystals for Dense Nuclear Matter and Neutron Stars

    hep-ph 2026-07 conditional novelty 7.0 of 10

    A crystal of holographic baryons in the Witten-Sakai-Sugimoto model yields a nuclear-matter equation of state compatible with neutron-star observations.

  2. Neutrino-induced hyperon final-state interactions as constraints on the in-medium hyperon potential

    nucl-th 2026-07 conditional novelty 7.0 of 10

    Neutrino hyperon final-state interactions at SBND/DUNE constrain the sub-saturation U_Λ and U_Σ potentials, mapping them through a GM1 EOS to a neutron-star maximum-mass posterior set mainly by external priors.

  3. Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase

    nucl-th 2026-06 unverdicted novelty 7.0 of 10

    Hybrid stars with a 2SC+⟨dd⟩ quark core cool hotter than with 2SC and near CFL; with a 3P2 gap near 5×10^8 K their cooling curves pass through the observed temperatures of 3C58, Vela Jr., and Vela-like pulsars.

  4. In-medium hyperon potentials and the quarkyonic hyperon onset: charged $\Sigma$'s in $\beta$-equilibrium and the neutrino connection

    nucl-th 2026-07 conditional novelty 6.5 of 10

    In-medium potentials give the quarkyonic hyperon onset weight-2 leverage on U_Y, ban Σ⁻ in β-equilibrium, keep TOV softening ≲0.025 M_⊙, and leave core strangeness prior-dominated once neutrino FSI pin U_Λ(n0).

  5. Accelerator neutrinos as a probe of in-medium hyperon potentials

    nucl-th 2026-07 conditional novelty 6.5 of 10

    StrangeMC forecasts that SBND/DUNE hyperon FSI observables constrain U_Λ(ρ0) to ~6 MeV after slope marginalization, with systematics distinct from hypernuclear data.

  6. Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    In relativistic mean field theory, a larger effective nucleon mass softens the supernova equation of state, yielding more compact proto-neutron stars, earlier black hole collapse, and higher-energy neutrino emission.

  7. On the Nucleon Effective Mass in Neutron Stars Cooling

    hep-th 2026-07 conditional novelty 6.0 of 10

    Using the Landau instead of the Dirac effective nucleon mass in neutron-star cooling calculations cools massive stars faster, changing predicted surface temperatures by ~0.03–0.06 dex.

  8. Black hole-neutron star binaries with high spins and large mass asymmetries: III. Properties of the ejected material and its electromagnetic signatures

    gr-qc 2026-07 conditional novelty 6.0 of 10

    High-spin, high-mass-ratio black hole–neutron star mergers eject 0.02–0.06 solar masses of neutron-rich (Y_e≈0.05) debris whose kilonovae are infrared-bright, optically dark, and match late-time AT2017gfo while stayin...

  9. Quarkyonic Stars with Strangeness

    nucl-th 2026-07 conditional novelty 6.0 of 10

    A three-flavor quarkyonic model with octet baryons yields stiffer neutron-star EOS and raises maximum masses, potentially resolving the hyperon puzzle.

  10. NNStar: An end-to-end AI agent for nuclear matter and neutron star physics

    nucl-th 2026-07 conditional novelty 6.0 of 10

    NNStar packages the RMF-to-neutron-star pipeline as a portable LLM-agent skill, validated on TM1/NL3/FSU-δ6.7 and demonstrated by an autonomous σ6-extended TM1 fit.

  11. Constraints on maximum neutron star mass from proto-neutron star evolution

    nucl-th 2025-05 conditional novelty 5.0 of 10

    Hyperonic neutron stars are inferred to cap at roughly 2.15 to 2.2 solar masses, while stars above 2.2 solar masses should have purely nucleonic cores.

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