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Nuclear Theory·nucl-th

Monday·September 26, 2022

5 papers—2 primary·3 cross-listed

All5Primary2Cross-lists3
  1. 03

    [Submitted on 22 Sept 2022] (cross-list from hep-ph)

    Resolving the Scales of the Quark-Gluon Plasma with Energy Correlators

    Carlota Andres🇫🇷 · Fabio Dominguez🇪🇸 · Raghav Kunnawalkam Elayavalli🇺🇸 · Jack Holguin🇫🇷 · Cyrille Marquet🇫🇷 · Ian Moult🇺🇸

    Jets provide us with ideal probes of the quark-gluon plasma (QGP) produced in heavy-ion collisions, since its dynamics at its different scales is imprinted into the multi-scale substructure of the final state jets. We present a new approach to jet substructure in heavy-ion collisions based on the study of correlation functions of energy flow operators. By analysing the two-point correlator of an in-medium quark jet, we demonstrate that the spectra of correlation functions robustly identify the scales defined by the properties of the QGP, particularly those associated with the onset of colour coherence.

    Comments:
    5 pages, 4 lovely figures. Minor changes, matches published PRL version
    Subjects:
    High Energy Physics — Phenomenology (hep-ph); High Energy Physics — Experiment (hep-ex); Nuclear Experiment (nucl-ex); Nuclear Theory (nucl-th)
    arXiv:
    2209.11236 [pdf]
    PRL(2023)·129 citations
  2. 04

    [Submitted on 23 Sept 2022] (cross-list from hep-ph)

    Production of exotic electromagnetic bound systems in ultra-peripheral heavy ion collisions with two-photon processes

    Gongming Yu🇨🇳 · Zhongxia Zhao · Yanbing Cai🇨🇳 · Quangui Gao🇨🇳 · Qiang Hu🇨🇳 · Haitao Yang

    We calculate the production of exotic electromagnetic bound systems, which ia an consisting of a () bound state system such as positronium, dimuonium, and ditauonium, by photon-photon interaction with the equivalent photon approximation in ultra-peripheral heavy ion collisions considering the nuclear form factor. The numerical results demonstrate that the experimental study of positronium, dimuonium, and ditauonium in ultra-peripheral collisions is feasible at Relativistic Heavy Ion Collider (RHIC) and Large Hadron Collider (LHC) energies.

    Comments:
    7 pages, 2 figures
    Subjects:
    High Energy Physics — Phenomenology (hep-ph); Nuclear Theory (nucl-th)
    arXiv:
    2209.11439 [pdf]
    8 citations
  3. 05

    [Submitted on 23 Sept 2022] (cross-list from astro-ph.HE)

    Accreting neutron stars from the nuclear energy-density functional theory. II. Equation of state and global properties

    A. F. Fantina🇫🇷 · J. L. Zdunik🇵🇱 · N. Chamel🇧🇪 · J. M. Pearson🇨🇦 · L. Suleiman🇵🇱 · S. Goriely🇧🇪

    The accretion of matter onto the surface of a neutron star in a low-mass X-ray binary triggers X-ray bursts, whose ashes are buried and further processed thus altering the composition and the properties of the stellar crust. In this second paper of a series, the impact of accretion on the equation of state and on the global properties of neutron stars is studied in the framework of the nuclear energy-density functional theory. Considering ashes made of Fe, we calculated the equations of state using the same Brussels-Montreal nuclear energy-density functionals BSk19, BSk20, and BSk21, as those already employed for determining the crustal heating in our previous study for the same ashes. All regions of accreting neutron stars were treated in a unified and thermodynamically consistent way. With these equations of state, we determined the mass, radius, moment of inertia, and tidal deformability of accreted neutron stars and compared with catalyzed neutron stars for which unified equations of state based on the same functionals are available. The equation of state of accreted neutron stars is found to be significantly stiffer than that of catalyzed matter, with an adiabatic index throughout the crust. For this reason, accreting neutron stars have larger radii. However, their crustal moment of inertia and their tidal deformability are hardly changed provided density discontinuities at the interface between adjacent crustal layers are properly taken into account. The enhancement of the stiffness of the equation of state of accreting neutron stars is mainly a consequence of nuclear shell effects, thus confirming the importance of a quantum treatment as stressed in our first study. With our previous calculations of crustal heating using the same functionals, we have thus obtained consistent microscopic inputs for simulations of accreting neutron stars.

    Comments:
    10 pages, 7 figures. The tables of the equations of state are available at the CDS
    Subjects:
    High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)
    arXiv:
    2209.11457 [pdf]
    Astron.Astrophys.(2022)·15 citations

Affiliations

first authorsco-authorsvia INSPIRE