Prafulla K. Panda

The effect of isoscalar–isovector coupling in infinite nuclear matter

In the framework of relativistic mean field theory, we study the effect of nonlinear cross coupling between the isoscalar–vector and isovector–vector mesons on top of G2 parametrization. The energy and pressure densities are calculated over a wide range of baryon densities. The observables such as symmetry energy and related coefficients are also evaluated systematically. The effect of cross coupling on the symmetry energy of symmetric nuclear matter is studied. The work is further extended to β-equilibrium matter to estimate the mass and radius of neutron stars and also to the baryon octet to see the effect of coupling over the equation of state.

SPIN POLARIZATION IN HIGH DENSITY QUARK MATTER

We investigate the occurrence of a ferromagnetic phase transition in high density hadronic matter (e.g., in the interior of a neutron star). This could be induced by a four-fermion interaction analogous to the one which is responsible for chiral symmetry breaking in the Nambu–Jona-Lasinio model, to which it is related through a Fierz transformation. Flavor SU(2) and flavor SU(3) quark matter are considered. A second-order phase transition is predicted at densities about 5 times the normal nuclear matter density. It is also found that in flavor SU(3) quark matter, a first-order transition from the so-called 2 flavor super-conducting phase to the ferromagnetic phase arises. The color-flavor-locked phase may be completely hidden by the FP.

Compact stars within a soft symmetry energy quark-meson-coupling model

We investigate compact star properties within the quark meson coupling model (QMC) with a soft symmetry energy density dependence at large densities. In particular, the hyperon content and the mass/radius curves for the families of stars obtained within the model are discussed. The hyperon-meson couplings are chosen according to experimental values of the hyperon nuclear matter potentials, and possible uncertainties are considered. It is shown that a softer symmetry energy gives rise to stars with less hyperons, smaller radii and larger masses. Hyperon-meson couplings may also have a strong effect on the mass of the star.

Hyperon stars in a modified quark meson coupling model

We determine the equation of state (EOS) of nuclear matter with the inclusion of hyperons in a self-consistent manner by using a modified quark meson coupling model where the confining interaction for quarks inside a baryon is represented by a phenomenological average potential in an equally mixed scalar-vector harmonic form. The hadron-hadron interaction in nuclear matter is then realized by introducing additional quark couplings to

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

\ensuremath{\sigma},\phantom{\rule{0.16em}{0ex}}\ensuremath{\omega}

Nuclear symmetry energy in a modified quark meson coupling model

, and

Nuclear pasta phases within the quark-meson coupling model

\ensuremath{\rho}

QMC approach based on the Bogoliubov independent quark model of the nucleon

mesons through mean-field approximations. The effect of a nonlinear

BCS Theory of Hadronic Matter at High Densities

\ensuremath{\omega}\text{\ensuremath{-}}\ensuremath{\rho}

The effect of isoscalar-isovector coupling in infinite nuclear matter

term on the EOS is studied. The hyperon couplings are fixed from the optical potential values and the mass-radius curve is determined satisfying the maximum mass constraint of