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Nuclear Theory·nucl-th

Wednesday·April 12, 2023

10 papers—3 primary·7 cross-listed

All10Primary3Cross-lists7
  1. 01

    Instruction of my personal computing library

    Tomohiro Oishi

    This document is prepared to introduce and explain how to use the computing library composed by T. Oishi. The library-01 TOSPEM solves, for the spherical nucleus, (i) the Schroedinger equation for the single-nucleon states within the Woods-Saxon potential, (ii-a) the electric or magnetic transition strength, B(EJ) or B(MJ), between the arbitrary set of initial and final states of the nucleus of interest, and (ii-b) Weisskopf estimate for comparison with results in (ii-a). The library-02 RESONA is composed to solve the resonant eigenstates of spherical Schroedinger equations. The final version is expected to be published for educational and commercial purposes. Before the official publication, under the agreement with publishers, I make the current, preliminary version open for public. Two applications, GFORTRAN and GNUPLOT, are necessary for full usage. Feedbacks and comments on products will be appreciated. The source codes etc. are available in the GitHub repository [1].

    nucl-thnucl-exquant-ph0 citations
  2. 02

    Multi-nucleon structure and dynamics via quantum computing

    Weijie Du🇺🇸 · James P. Vary🇺🇸

    We propose a framework for computing the structure and dynamics for second-quantized many-nucleon Hamiltonians on quantum computers. We develop an oracle-based Hamiltonian input model that computes the many-nucleon states and nonzero Hamiltonian matrix elements of the many-nucleon system. With our Fock-state based input model, we show how to implement the sparse matrix simulation algorithms to calculate the dynamics of the second-quantized many-nucleon Hamiltonian. Based on the dynamics simulation methods, we also present the methodology for structure calculations of the many-nucleon system. In this work, we provide an explicit circuit design of our input model of the second-quantized Hamiltonian within a direct encoding scheme that maps the occupation of each available single-particle state in the many-nucleon state to the state of specific qubit in a quantum register. We analyze our method and provide the asymptotic cost in computing resources for structure and dynamics calculations of many-nucleon systems. For pedagogical purposes, we demonstrate our input model with two model problems in restricted model spaces.

    nucl-thquant-phPRA·14 citations
  3. 03

    Investigating Dark Matter-Admixed Neutron Stars with NITR Equation of State in Light of PSR J0952-0607

    Pinku Routaray🇮🇳 · Sailesh Ranjan Mohanty🇮🇳 · H.C. Das🇮🇳 · Sayantan Ghosh🇮🇳 · P.J. Kalita🇮🇳 · V. Parmar🇮🇳 · Bharat Kumar🇮🇳

    The fastest and heaviest pulsar, PSR J0952-0607, with a mass of , has recently been discovered in the disk of the Milky Way Galaxy. In response to this discovery, a new RMF model, `NITR' has been developed. The NITR model's naturalness has been confirmed by assessing its validity for various finite nuclei and nuclear matter properties, including incompressibility, symmetry energy, and slope parameter values of 225.11, 31.69, and 43.86 MeV, respectively. These values satisfy the empirical/experimental limits currently available. The maximum mass and canonical radius of a neutron star (NS) calculated using the NITR model parameters are 2.355 and 13.13 km, respectively, which fall within the range of PSR J0952-0607 and the latest NICER limit. This study aims to test the consistency of the NITR model by applying it to various systems. As a result, its validity is extensively calibrated, and all the nuclear matter and NS properties of the NITR model are compared with two established models such as IOPB-I and FSUGarnet. In addition, the NITR model equation of state (EOS) is employed to obtain the properties of a dark matter admixed NS (DMANS) using two approaches (I) single-fluid and (II) two-fluid approaches. In both cases, the EOS becomes softer due to DM interactions, which reduces various macroscopic properties such as maximum mass, radius, tidal deformability, etc. The various observational data such as NICER and HESS are used to constrain the amount of DM in both cases. Moreover, we discuss the impact of dark matter (DM) on the nonradial -mode frequency of the NS in a single fluid case only and try to constrain the amount of DM using different theoretical limits available in the literature.

    nucl-thJCAP(2023)·44 citations

Affiliations

first authorsco-authorsvia INSPIRE