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Nuclear Theory·nucl-th

Monday·December 23, 2024

10 papers—2 primary·8 cross-listed

All10Primary2Cross-lists8
  1. 01

    Quark-Quark and Quark-nucleon Potential model Extended-soft-core meson-exchange Interactions

    Th. A. Rijken🇳🇱 · Y. Yamamoto🇯🇵

    The Quark-quark (QQ) and Quark-nucleon (QN) interactions in this paper are derived from the Extended-soft-core (ESC) interactions. The meson-quark-quark (MQQ) vertices are determined in the framework of the constituent quark model (CQM). These vertices are such that upon folding with the ground-state baryon quark wave functions the one-boson-exchange (OBE) amplitudes for baryon-baryon (BB), and in particularly for nucleon-nucleon (NN), are reproduced. This opens the attractive possibility to define meson-quark interactions at the quark level which are directly related related to the interactions at the baryon level. the latter have been determined by the baryon-baryon data. Application of these "realistic" quark-quark interactions in the quark-matter phase is presumably of relevance for the description of highly condensed matter, as e.g. neutron-star matter.

    nucl-thhep-ph2 citations
  2. 02

    Constraining neutron star properties through parity-violating electron scattering experiments and relativistic point coupling interactions

    P.S. Koliogiannis🇭🇷 · E. Yuksel🇬🇧 · N. Paar🇭🇷

    Parity-violating electron scattering experiments on (CREX) and (PREX-2) offer valuable insight into the isovector properties of finite nuclei, providing constraints for the density dependence of the nuclear equation of state, which is crucial for understanding astrophysical phenomena. In this work, we establish functional dependencies between the properties of finite nuclei-such as weak charge form factors and neutron skin thickness-and the bulk properties of neutron stars, including tidal deformability from binary neutron star mergers and neutron star radii. The dependencies are formulated by introducing a family of -equilibrated equations of state based on relativistic energy density functionals with point coupling interactions. The charge minus the weak form factors derived from CREX and PREX-2 measurements, combined with the observational constraints on tidal deformability from the GW170817 event, are used to constrain the symmetry energy and neutron star radii. Notably, the energy density expanded up to the fourth order in symmetry energy yields larger radii compared to calculations limited to the second order term. However, the results reveal a discrepancy between the constraints provided by the CREX and PREX-2 experiments. For a more quantitative assessment, higher precision parity-violating electron scattering data and neutron star observations are required.

    nucl-thastro-ph.HEastro-ph.SRnucl-exPLB(2025)·5 citations

Affiliations

first authorsco-authorsvia INSPIRE