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Nuclear Theory·nucl-th

Friday·June 27, 2025

5 papers—3 primary·2 cross-listed

All5Primary3Cross-lists2
  1. 04

    Iterative Harrow-Hassidim-Lloyd quantum algorithm for solving resonances with eigenvector continuation

    Hantao Zhang🇨🇳 · Dong Bai🇨🇳 · Zhongzhou Ren🇨🇳

    We propose a novel quantum algorithm for solving nuclear resonances, which is based on the iterative Harrow-Hassidim-Lloyd algorithm and eigenvector continuation with complex scaling. To validate this approach, we compute the resonant states of system and achieve results in good agreement with traditional methods. Our study offers a new perspective on calculating eigenvalues of non-Hermitian operators and lays some groundwork for further exploration of nuclear resonances using quantum computing.

    ↳ quant-phnucl-thPLB(2026)·3 citations
  2. 05

    Proto-neutron Stars with Dark Matter Admixture: A Single-Fluid Approach

    Adamu Issifu🇧🇷 · Débora P. Menezes🇧🇷 · Tobias Frederico🇧🇷

    This work investigates the impact of dark matter (DM) on the microscopic and macroscopic properties of proto-neutron stars (PNSs). We employ a single-fluid framework in which DM interacts with ordinary matter (OM) via the Higgs portal and remains in thermal equilibrium through non-gravitational interactions. Using a quasi-static approximation, we analyze the evolution of PNSs during the Kelvin-Helmholtz phase by varying the DM mass while keeping the entropy per baryon and lepton fraction fixed. Our results show that DM absorbs thermal energy from the stellar medium without efficient re-emission, thereby altering neutrino emission and affecting the star's thermal evolution history. Furthermore, neutrinos contribute significantly to pressure support in the PNS phase, inhibiting DM mass accretion during neutrino-trapped stages. Based on the requirement to satisfy the observed neutron star mass constraint and to maintain consistency with supernova remnant data, we suggest an upper limit of for the DM mass that can accrete in evolving PNSs, within the model framework. In contrast, we established that cold neutron stars (NSs) can support higher DM masses without compromising equilibrium stability, owing to increased central density, enhanced gravitational binding energy, and reduced thermal pressure.

    ↳ astro-ph.HEnucl-thPhys.Dark Univ.(2025)·8 citations

Affiliations

first authorsco-authorsvia INSPIRE