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Nuclear Theory·nucl-th

Friday·March 28, 2025

9 papers—3 primary·6 cross-listed

All9Primary3Cross-lists6
  1. 01

    Heavy Neutron Star Phenomenology with an H-dibaryon

    Jesper Leong🇦🇺 · Anthony W. Thomas🇦🇺 · Pierre A. M. Guichon🇦🇺

    The equation of state for dense nuclear matter in -equilibrium is explored including the possibility of a doubly-strange H-particle. Consistent with experimental constraints, the mass of the H in free space is taken to be near the threshold. Within the quark-meson coupling model, which we use, no new parameters are required to describe the interaction between the H-dibaryon and the other baryons. The maximum mass is only slightly reduced, and the tidal deformability is essentially unchanged with this addition. In heavy neutron stars the H is abundant and extends as far as 6 km from the center of the core.

    nucl-thastro-ph.HEhep-phPRC(2026)·2 citations
  2. 02

    Are Neutron Stars Rich in H-dibaryons?

    Jesper Leong · Anthony W. Thomas · Pierre A. M. Guichon

    The possible existence of an H-dibaryon near the threshold has still not been decided experimentally. This raises the question of the potential effects on neutron stars if it does exist. We explore the consequences within the quark-meson coupling model, using the excluded volume formalism. While the H is abundant in heavy stars the maximum mass is only lowered slightly by its presence.

    nucl-thastro-ph.HEhep-phPoS(2025)·1 citation
  3. 03

    Superfluid density in linear response theory : pulsar glitches from the inner crust of neutron stars

    Giorgio Almirante🇫🇷 · Michael Urban🇫🇷

    The question of whether there are enough superfluid neutrons in the inner crust of neutron stars to explain pulsar glitches remains a topic of debate. Previous band structure calculations suggest that the entrainment effect significantly reduces the superfluid density. In this letter, a new derivation of the BCS expression for the superfluid density is given. We compute it in the superfluid band theory framework through linear response theory, for a small relative velocity between superfluid and normal components, under the assumption that the pairing gap in the rest frame of the superfluid is constant and not affected by the perturbation. Our result suggests that a formula extensively used in neutron star physics is incomplete. Numerical evaluations for two realistic configurations reveal that the previously neglected contribution drastically alters the picture of the superfluid reservoir in the inner crust of neutron stars, suggesting that about 90% of the neutrons are effectively superfluid.

    nucl-thcond-mat.quant-gasPRL(2025)·14 citations

Affiliations

first authorsco-authorsvia INSPIRE