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Nuclear Theory·nucl-th

Monday·April 5, 2021

5 papers—2 primary·3 cross-listed

All5Primary2Cross-lists3
  1. 01

    Dynamical evolution of magnetic field in the pre-equilibrium quark-gluon plasma

    Li Yan🇨🇳 · Xu-Guang Huang🇨🇳

    High-energy heavy-ion collisions generate extremely strong magnetic field which plays a key role in a number of novel quantum phenomena in quark-gluon plasma (QGP), such as the chiral magnetic effect (CME). However, due to the complexity in theoretical modellings of the coupled electromagnetic fields and the QGP system, especially in the pre-equilibrium stages, the lifetime of the magnetic field in the QGP medium remains undetermined. We establish, for the first time, a kinetic framework to study the dynamical decay of the magnetic field in the early stages of a weakly coupled QGP by solving the coupled Boltzmann and Maxwell equations. We find that at late times a magnetohydrodynamical description of the coupled system emerges. With respect to realistic collisions at RHIC and the LHC, we estimate the residual strength of the magnetic field in the QGP when the system start to evolve hydrodynamically.

    nucl-thhep-phnucl-exPRD(2023)·65 citations
  2. 02

    Influence of non-statistical properties in nuclear structure on emission of prompt fission neutrons

    Toshihiko Kawano🇺🇸 · Shin Okumura🇦🇹 · Amy E. Lovell🇺🇸 · Ionel Stetcu🇺🇸 · Patrick Talou🇺🇸

    The Hauser-Feshbach Fission Fragment Decay (HFD) model is extended to calculate the prompt fission neutron spectrum (PFNS) for the thermal neutron induced fission on U, where the evaporated neutrons from all possible fission fragment pairs are aggregated. By studying model parameter sensitivities on the calculated PFNS, as well as non-statistical behavior of low-lying discrete level spin distribution, we conclude that discrepancies between the aggregation calculation and the experimental PFNS seen at higher neutron emission energies can be attributed to both the primary fission fragment yield distribution and the possible high spin states that are not predicted by the statistical theory of nuclear structure.

    nucl-thPRC(2021)·8 citations
  3. 03

    Magnetic monopole in a chiral plasma: chiral dyon

    Michael Lublinsky🇮🇱 · Jared Reiten🇺🇸 · Andrey V. Sadofyev🇪🇸

    The placement of a magnetic monopole into an electrically-neutral chiral plasma with a non-zero axial density results in an electric polarization of the matter. The electric current produced by the chiral magnetic effect is balanced by charge diffusion and Ohmic dissipation, which generates a non-trivial charge distribution. In turn, the latter induces a separation of chiralities along the magnetic field of the monopole due to the chiral separation effect. We find the stationary states of such a system, with vanishing total electric current and stationary axial current balanced by the chiral anomaly. In this solution, the monopole becomes "dressed" with an electric charge that is proportional to the averaged chiral density of the matter -- forming a chiral dyon. The interplay between the chiral effects on the one hand, and presence of magnetic field of the monopole on the other, may affect the evolution of the monopole density in the early Universe, contribute to the process of baryogenesis, and can also be instrumental for detection of relic monopoles using chiral materials.

    ↳ hep-phhep-thnucl-thPRD(2021)·0 citations
  4. 04

    Equation of State table with hyperon and antikaon for supernova and neutron star merger

    Tuhin Malik🇮🇳 · Sarmistha Banik🇮🇳 · Debades Bandyopadhyay🇮🇳

    We develop a new equation of state (EoS) table involving thermal (anti)kaons, Bose-Einstein condensate of mesons and -hyperons for core-collapse supernova and neutron star merger simulations. This EoS table is based on a finite temperature density-dependent relativistic hadron field theory where baryon-baryon interaction is mediated by scalar , vector and mesons, using the parameter set DD2 for nucleons. The repulsive hyperon-hyperon interaction is mediated by an additional strange meson. The EoS for the condensed matter is also calculated within the framework of relativistic mean field model, whereas the low-density, inhomogeneous matter is calculated in the extended Nuclear Statistical Equilibrium model (NSE). The EoS table is generated for a wide range of values of three parameters - baryon density ( to 1 fm), positive charge fraction(0.01 to 0.60) and temperature(0.1 to 158.48 MeV).

    ↳ astro-ph.HEnucl-thApJ(2021)·33 citations

Affiliations

first authorsco-authorsvia INSPIRE