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Nuclear Theory·nucl-th

Monday·March 17, 2025

10 papers—4 primary·6 cross-listed

All10Primary4Cross-lists6
  1. 01

    [Submitted on 13 Mar 2025]

    Energy rates due to Fe isotopes during presupernova evolution of massive stars

    Jameel-Un Nabi · Asim Ullah · Majid Iqbal

    This work presents the microscopic calculation of energy rates ({\gamma} ray heating and (anti)neutrino cooling rates) due to weak decay of selected Fe isotopes. The isotopes have astrophysical significance during the presupernova evolution of massive stars. The energy rates are calculated using the pn QRPA model and compared with the independent particle model (IPM), large scale shell model (LSSM) and recent shell model calculation (GXPF1J). The reported (anti)neutrino cooling rates are smaller by up to two orders of magnitude at low core temperature values than the IPM rates. The two calculations compare well at T = 30 GK. The comparison of cooling rates with the LSSM is interesting. The pn QRPA cooling rates due to even even Fe isotopes are smaller (up to 2 orders of magnitude). For the odd A isotopes, the reported rates are bigger up to an order of magnitude. The pn QRPA computed cooling rates are, up to 2 orders of magnitude, bigger when compared with the GXPF1J calculation. The {\gamma} ray heating rates due to electron capture rates rise with the temperature and density values of the stellar core. On the other hand, the {\gamma} ray heating due to \b{eta} decay increases with the core temperature values but decreases by orders of magnitude when the stellar core stiffens. The pn QRPA computed {\gamma} heating rates are bigger (up to 3 orders of magnitude) at high temperatures and densities (for the case of 55 56Fe) when compared with the recent shell model results. Owing to the importance of energy rates, this study may contribute to a realistic simulation of presupernova evolution of massive stars.

    Comments:
    25 Pages, 4 Tables, 7 Figures
    Subjects:
    Nuclear Theory (nucl-th)
    arXiv:
    2503.10951 [pdf]
    New Astron.(2024)·0 citations
  2. 02

    [Submitted on 14 Mar 2025]

    Systematic calculation on alpha decay and cluster radioactivity of superheavy nuclei

    Xuanpeng Xiao · Panpan Qi · Gongming Yu · Haitao Yang · Qiang Hu

    In the Coulomb and Proximity Potential Model (CPPM) framework, we have investigated the cluster radioactivity and alpha decay half-lives of superheavy nuclei. We study 22 different versions of proximity potential forms that have been proposed to describe proton radioactivity, two-proton radioactivity, heavy-ion radioactivity, quasi-elastic scattering, fusion reactions, and other applications. The half-lives of cluster radioactivity and alpha decay of 41 atomic nuclei ranging from 221Fr to 244Cm were calculated, and the results indicate that the refined nuclear potential named BW91 is the most suitable proximity potential form for the cluster radioactivity and alpha decay of superheavy nuclei since the root-mean-square (RMS) deviation between the experimental data and the relevant theoretical calculation results is the smallest ({\sigma}= 0.841). By using CPPM, we predicted the half-lives of 20 potential cluster radioactivity and alpha decay candidates. These cluster radioactivities and alpha decays are energetically allowed or observable but not yet quantified in NUBASE2020.

    Comments:
    20 pages, 2 figures, 6 tables
    Subjects:
    Nuclear Theory (nucl-th)
    arXiv:
    2503.10987 [pdf]
    0 citations
  3. 03

    [Submitted on 14 Mar 2025]

    Triple-charmed Hadron from Coalescence in Relativistic Heavy-Ion Collisions

    Tianyang Li🇨🇳 · Jiamin Liu🇨🇳 · Shiqi Zheng🇺🇸 · Baoyi Chen🇨🇳

    We investigate the production of the baryon in relativistic heavy-ion collisions. Unlike proton-proton collisions, nuclear collisions produce both deconfined matter and abundant charm quark pairs, which can coalesce to form the baryon, thereby significantly enhancing its production. We employ the Langevin model and the Instantaneous Coalescence Model (LICM), coupled with hydrodynamic simulations, to study charm quark diffusion and coalescence into the baryon in expanding QCD matter. The production of the is governed by the charm quark densities and the in-medium wavefunctions of the , which determines the coalescence probability for the three charm quarks. We calculate the production with realistic charm diffusions and different in-medium wave functions of baryon. We find that the production of the baryon is sensitive to these factors, which aids in understanding its properties in the hot QCD medium.

    Comments:
    7 pages, 3 figures
    Subjects:
    Nuclear Theory (nucl-th); High Energy Physics — Phenomenology (hep-ph)
    arXiv:
    2503.11223 [pdf]
    PLB(2025)·1 citation
  4. 04

    [Submitted on 14 Mar 2025]

    Scaling and universality in strange quark stars

    G. Lugones🇧🇷 · A. G. Grunfeld🇦🇷

    We derive scaling laws that connect certain macroscopic observables of strange quark stars with key microscopic properties of self-bound quark matter, such as the energy per baryon at zero pressure and the strength of repulsive interactions. We also identify universal relations linking global properties of strange quark stars - specifically, their moment of inertia, tidal deformability, and both gravitational and baryonic compactness. Remarkably, these relations hold for two substantially different microscopic models - the quark-mass density-dependent model with excluded-volume corrections and the vector MIT bag model - underscoring their robust, model-independent nature. We demonstrate that the universal relations for strange quark stars differ significantly from those previously established for neutron stars composed of hadronic matter, thus enabling discrimination between the two types of objects without requiring detailed knowledge of their equations of state. Moreover, observational constraints on the maximum mass of compact stars could place bounds on both the depth of quark-matter self-binding and the strength of quark repulsive interactions.

    Subjects:
    Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR); High Energy Physics — Phenomenology (hep-ph)
    arXiv:
    2503.11515 [pdf]
    PRD(2025)·5 citations

Affiliations

first authorsco-authorsvia INSPIRE