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Nuclear Theory·nucl-th

Wednesday·July 31, 2019

9 papers—3 primary·6 cross-listed

All9Primary3Cross-lists6
  1. 01

    [Submitted on 30 Jul 2019]

    Hadron matter in neutron stars in view of gravitational wave observations

    Felipe J. Llanes-Estrada🇪🇸 · Eva Lope-Oter (Universidad Complutense de Madrid)🇪🇸

    In this review we highlight a few physical properties of neutron stars and their theoretical treatment inasmuch as they can be useful for nuclear and particle physicists concerned with matter at finite density (and newly, temperature). Conversely, we lay out some of the hadron physics necessary to test General Relativity with binary mergers including at least one neutron star, in view of the event GW170817: neutron stars and their mergers reach the highest matter densities known, offering access to the matter side of Einstein's equations. In addition to minimum introductory material for those interested in starting research in the field of neutron stars, we dedicate quite some effort to a discussion of the Equation of State of hadron matter in view of gravitational wave developments; we address phase transitions and how the new data may help; we show why transport is expected to be dominated by turbulence instead of diffusion through most if not all of the star, in view of the transport coefficients that have been calculated from microscopic hadron physics; and we relate many of the interesting physics topics in neutron stars to the radius and tidal deformability.

    Comments:
    Review with 61 plots and sketches, 90 pages in preprint format, 7MB file size, meant for Progress in Particle and Nuclear Physics
    Subjects:
    Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)
    arXiv:
    1907.12760 [pdf]
    PPNP(2019)·24 citations
  2. 02

    [Submitted on 30 Jul 2019]

    Production of multi-charmed hadrons by recombination in heavy ion collisions

    Sungtae Cho🇰🇷 · Su Houng Lee🇰🇷

    We study the production of multi-charmed hadrons by recombination in heavy ion collisions by focusing on the production of , , , , baryons and X(3872) mesons. Starting from the estimation of yields for those hadrons at chemical freeze-out in both the statistical and coalescence model, we evaluate their transverse momentum distributions at mid-rapidity in the coalescence model. We show that yields of multi-charmed hadrons in heavy ion collisions at RHIC and LHC are large enough, and thereby not only multi-charmed hadrons observed so far, e.g., the but also those which have not been observed yet, can be discovered sufficiently in heavy ion collisions. We also find that the transverse momentum distribution ratio between various multi-charmed hadrons sensitively reflects the interplay between quark contents of corresponding hadrons as well as the transverse momentum distribution of charm quarks at the hadronization point, and therefore we insist that studying both the transverse momentum distributions of multi-charmed hadrons themselves and transverse momentum distribution ratios between various multi-charmed hadrons provide us with useful information on hadron production mechanism involving charm quarks in heavy ion collisions.

    Comments:
    20 pages, 9 figures
    Subjects:
    Nuclear Theory (nucl-th); High Energy Physics — Phenomenology (hep-ph); Nuclear Experiment (nucl-ex)
    arXiv:
    1907.12786 [pdf]
    PRC(2020)·29 citations
  3. 03

    [Submitted on 30 Jul 2019]

    Domain walls in neutron superfluids in neutron stars

    Shigehiro Yasui🇯🇵 · Muneto Nitta🇯🇵

    We work out domain walls in neutron superfluids realized in the core of neutron stars. Adopting the Ginzburg-Landau (GL) theory as a bosonic low-energy effective theory, we consider configurations of domain walls interpolating ground states, i.e., the uniaxial nematic (UN), D-biaxial nematic (D-BN), and D-biaxial nematic (D-BN) phases in the presence of zero, small and large magnetic fields, respectively. We solve the Euler-Lagrange equation from the GL free energy density, and calculate surface energy densities of the domain walls. We find that one extra Nambu-Goldstone mode is localized in the vicinity of a domain wall in the UN phase while a U(1) symmetry restores in the vicinity of one type of domain wall in the D-BN phase and all domain walls in the D-BN phase. Considering a pile of domain walls in the neutron stars, we find that the most stable configurations are domain walls perpendicular to the magnetic fields piled up in the direction along the magnetic fields in the D-BN and D-BN phases. We estimate the energy released from the deconstruction of the domain walls in the edge of a neutron star, and show that it can reach an astrophysical scale such as glitches in neutron stars.

    Comments:
    31 pages, 12 figures
    Subjects:
    Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics — Phenomenology (hep-ph); High Energy Physics — Theory (hep-th)
    arXiv:
    1907.12843 [pdf]
    PRC(2020)·17 citations

Affiliations

first authorsco-authorsvia INSPIRE