Neutron star, $\beta$-stable ring-diagram equation of state and Brown-Rho scaling

Abstract

Neutron star properties, such as its mass, radius, and moment of inertia, are calculated by solving the Tolman-Oppenheimer-Volkov (TOV) equations using the ring-diagram equation of state (EOS) obtained from realistic low-momentum NN interactions $V_{low-k}$. Several NN potentials (CDBonn, Nijmegen, Argonne V18 and BonnA) have been employed to calculate the ring-diagram EOS where the particle-particle hole-hole ring diagrams are summed to all orders. The proton fractions for different radial regions of a $\beta$-stable neutron star are determined from the chemical potential conditions ${\mu }_n-{\mu }_p={\mu }_e={\mu }_{\mu }$. The neutron star masses, radii and moments of inertia given by the above potentials all tend to be too small compared with the accepted values. Our results are largely improved with the inclusion of medium corrections based on Brown-Rho scaling where the in-medium meson masses, particularly those of $\omega$, $\rho$ and $\sigma$, are slightly decreased compared with their in-vacuum values. Representative results using such medium corrected interactions are neutron star mass $M\sim 1.8M_{\odot }$, radius $R\sim 9$ km and moment of inertia $\sim 60M_{\odot }k{m}^2$. The mass-radius trajectories given by the above four realistic NN potentials are by and large overlapping.

12.7 pages, 13 figures, 3 tables

References in corpus (7)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Pulsars as Astrophysical Laboratories for Nuclear and Particle Physics
• Locating the inner edge of neutron star crust using terrestrial nuclear laboratory data
• The Neutron Star Crust: Nuclear Physics Input
• Shell model description of the 14C dating beta decay with Brown-Rho-scaled NN interactions
• Low-momentum NN interactions and all-order summation of ring diagrams of symmetric nuclear matter
• Low-momentum ring diagrams of neutron matter at and near the unitary limit

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• Scale-Invariant Hidden Local Symmetry, Topology Change and Dense Baryonic Matter
• A pseudo-conformal structure in dense baryonic matter
• A New Approach to Physics of Nuclei
• Imprints of Nuclear Symmetry Energy on Properties of Neutron Stars
• Topology change, emergent symmetries and compact star matter
• Low-momentum interactions with Brown-Rho-Ericson scalings and the density dependence of the nuclear symmetry energy
• Unitarity potentials and neutron matter at the unitary limit
• Introduction to low-momentum effective interactions with Brown-Rho scaling and three-nucleon forces
• Compact Star Matter: EoS with New Scaling Law
• Origins and Impacts of High-Density Symmetry Energy
• Nucleon-anti-nucleon intruder state of Dirac equation for nucleon in deep scalar potential well