PaperPanorama

Nuclear Theory·nucl-th

Monday·October 28, 2019

6 papers2 primary·4 cross-listed

  1. 01

    Third order viscous hydrodynamics from the entropy four current

    Mohammed Younus🇿🇦 · Azwinndini Muronga🇿🇦

    Non-equilibrium dynamics for relativistic fluid or quark gluon plasma (QGP) have already been calculated earlier upto third order using both kinetic and thermodynamic approaches. Calculations presented in this manuscript are based on thermodynamics principles. The expressions for third order dissipative fluxes have been derived from equation for entropy 4-current developed earlier by A. Muronga. The relaxation equations in the present work have been developed in a simple Bjorken (1+1)D scenario and Eckart frame. The relaxation equations are found to have slightly different values for the coupling coefficients as compared to calculations from earlier models. The solutions to the differential equations have been found to be sensitive to values of these coefficients. The shear relaxation equations derived in third order theory are discussed term by term. Effects of third order theory on shear relaxation time has been discussed. Thermodynamic quantities related to hot and dense matter have been calculated as functions of proper time. Moreover, various initial conditions for the relaxation equations have been assumed to study their effects on above mentioned observables. A LHC QGP formation time of = 0.4 fm/c and temperature of T = 500 MeV have been assumed.

    nucl-thPRC(2020)·9 citations
  2. 02

    The properties of neutron star from realistic nucleon-nucleon interaction within relativistic Hartree-Fock model

    Ying Zhang · Peng Liu · Jinniu Hu

    The properties of neutron star are studied in the framework of relativistic Hartree-Fock (RHF) model with realistic nucleon-nucleon () interactions, i.e. Bonn potentials. The strong repulsion of interaction at short range is properly removed by the unitary correlation operator method (UCOM). Meanwhile, the tensor correlation is neglected due to the very rich neutron environment in neutron star, where the total isospin of two nucleons can be approximately regarded as . The equations of state of neutron star matter are calculated in equilibrium and charge neutrality conditions. The properties of neutron star, such as mass, radius, and tidal deformability are obtained by solving the Tolman-Oppenheimer-Volkoff equation and tidal equation. The maximum masses of neutron from Bonn A, B, C potentials are around . The radius are km at , respectively. The corresponding tidal deformabilities are . All of these properties are satisfied the recent observables from the astronomical and gravitational wave devices and are consistent with the results from the relativistic Brueckner-Hartree-Fock model.

    nucl-thIJMPE(2020)·2 citations

Affiliations

first authorsco-authorsvia INSPIRE