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Nuclear Theory·nucl-th

Monday·February 12, 2018

5 papers—3 primary·2 cross-listed

All5Primary3Cross-lists2
  1. 01

    Nuclear reaction path and requantization of TDDFT

    Kai Wen · Takashi Nakatsukasa

    Using a theory of large amplitude collective motion, the adiabatic self-consistent collective coordinate method, we derive reaction path for the fusion process at sub-barrier energies. The collective Hamiltonian to describe the fusion process is constructed, based on the obtained reaction path and canonical variables. We study the reaction of N=Z stable nuclei, alpha+16O, 16O+16O, and alpha+12C. The results suggest that, after two nuclei touch, the reaction path is significantly deviated from the simple relative motion, which may affect the deep sub-barrier fusion cross section.

    nucl-thJPS Conf.Proc.(2018)·1 citation
  2. 02

    Vector-Interaction-Enhanced Bag Model

    Mateusz Cierniak🇵🇱 · Thomas Klähn🇺🇸 · Tobias Fischer🇵🇱 · Niels-Uwe Bastian🇵🇱

    A commonly applied quark matter model in astrophysics is the thermodynamic bag model (tdBAG). The original MIT bag model approximates the effect of quark confinement, but does not explicitly account for the breaking of chiral symmetry, an important property of Quantum Chromodynamics (QCD). It further ignores vector repulsion. The vector-interaction-enhanced bag model (vBag) improves the tdBAG approach by accounting for both dynamical chiral symmetry breaking and repulsive vector interactions. The latter is of particular importance to studies of dense matter in beta-equilibriumto explain the two solar mass maximum mass constraint for neutron stars. The model is motivated by analyses of QCD based Dyson-Schwinger equations (DSE), assuming a simple quark-quark contact interaction. Here, we focus on the study of hybrid neutron star properties resulting from the application of vBag and will discuss possible extensions.

    nucl-thastro-ph.HEhep-phUniverse(2018)·24 citations
  3. 03

    Moments of inertia of neutron stars in relativistic mean field theory: the role of the isovector scalar channel

    Zhuang Qian🇨🇳 · Ruo Yu Xing🇨🇳 · Bao Yuan Sun🇨🇳

    With the inclusion of the isovector scalar channel in the meson-nucleon couplings, taking DD-ME as an effective interaction, the moments of inertia of neutron stars possessing various stellar masses are studied within the density dependent relativistic mean field (RMF) theory. The isovector scalar channel contributes to the softening of the neutron-star matter equation of state (EOS) and therefore the reduction of the maximum mass and radius of neutron stars. Smaller values of the total moment of inertia and the crustal moment of inertia are then obtained in DD-ME via numerical procedure in comparison with those in other selected RMF functionals. In addition, the involvement of the isovector scalar channel lowers the thickness of the neutron star crust and its mass fraction as well. The sensitivity to both the crustal mass and stellar radius causes the crustal moment of inertia to be more obviously reduced than the total one, eventually leading to a suppression on the fraction of crustal moment of inertia in DD-ME. The results indicate the crustal moment of inertia as a more sensitive probe of the neutron-star matter EOS than the total one, and demonstrate that the isovector scalar meson-nucleon couplings in the RMF theory could exert influence over the physics of pulsar glitches.

    nucl-thastro-ph.HE7 citations

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first authorsco-authorsvia INSPIRE