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Nuclear Theory·nucl-th

Friday·October 24, 2025

7 papers—4 primary·3 cross-listed

All7Primary4Cross-lists3
  1. 05

    Impact of the nuclear equation of state on the explodability of massive stars

    Jade Powell · Bernhard Müller🇦🇺

    In recent years, astrophysical observations have placed tight constraints on key properties of the nuclear equation of state (EoS). Using 93 two-dimensional simulations for three different EoS compatible with the current tight constraints, we show that the EoS remains a major uncertainty for the outcome of core-collapse supernovae. Whereas explosions are obtained in most cases for the SFHo and SFHx EoS, for the CMF EoS, which includes a crossover from nucleonic matter to a quark phase, explosions occur only for 2 out of 15 progenitors. Less favourable conditions for neutrino-driven explosions arise for the CMF EoS due to lower neutrino luminosities and mean energies and slightly weaker contraction of the warm proto-neutron star. Our results suggest that the explodability of massive stars cannot yet be predicted based on first principles without better knowledge of the nuclear EoS. Conversely, observational constraints on stellar explodability may help further constrain the EoS.

    ↳ astro-ph.HEnucl-thPRD(2026)·12 citations
  2. 06

    Probing the Three-dimension Emission Source and Neutron Skin via - Correlations in Heavy-Ion Collisions

    Haojie Zhang🇨🇳 · Junhuai Xu🇨🇳 · Pengcheng Li🇨🇳 · Zhi Qin🇨🇳 · Dawei Si🇨🇳 · Yijie Wang🇨🇳 · Yongjia Wang🇨🇳 · Qingfeng Li🇨🇳 · Zhigang Xiao🇨🇳

    The Richardson-Lucy algorithm is applied to reconstruct the three-dimensional source function of identical pions from their two-particle correlation functions. The algorithm's performance is first evaluated through simulations with Gaussian-type initial source functions. Its imaging quality and robustness are further demonstrated with experimental data from Au+Au collisions at 1.23 A GeV, collected by the HADES Collaboration. Additionally, using UrQMD simulations of Pb+Pb collisions at 1.5 A GeV, we show that the deblurred source functions exhibit sensitivity to the initial neutron skin thickness of the colliding nuclei. This highlights the potential of the Richardson-Lucy algorithm as a tool for probing the neutron density distribution in heavy nuclei.

    ↳ nucl-exnucl-thPRC(2026)·4 citations
  3. 07

    A Microphysical Probe of Neutron Star Interiors: Constraining the Equation of State with Glitch Dynamics

    Zhonghao Tu🇨🇳 · Ang Li🇨🇳

    Glitches in neutron stars originate from the sudden transfer of angular momentum between superfluid components and the observable crust. By modeling this glitch dynamics--including vortex motion, mutual friction, and angular momentum exchange--one may hope to probe the dense matter equation of state. In this work, we explore, within a highly idealized three-component framework, whether the glitch rise could in principle carry information about microphysical inputs such as entrainment and mutual friction. We compute the glitch rise in response to self-consistently calculated microphysical parameters (pinning and mutual friction) based on unified equations of state, and compare theoretical predictions of the overshoot patterns and timing residuals to the 2016 Vela glitch. Within this specific framework, the models favor crustal superfluid coupling on timescales of order s, overshoot behavior in the core associated with relatively strong central mutual friction, and rise times consistent with the observed upper limit of 12.6 s. Using a Markov Chain Monte Carlo analysis of the timing residuals, we then map the regions of parameter space that are compatible with the data under our adopted assumptions. Our analysis favors comparatively weak entrainment in the inner crust and an overall core mutual friction that is weaker than that in the inner crust. These exploratory results demonstrate that, under such restrictive assumptions, glitch-rise morphology is sensitive to microphysical inputs and that future high-cadence timing observations, interpreted with more realistic dynamical models, could potentially help constrain the internal dynamics and composition of neutron stars.

    ↳ astro-ph.HEastro-ph.SRnucl-thApJ(2026)·1 citation

Affiliations

first authorsco-authorsvia INSPIRE