Isospin dependence of entrainment in superfluid neutron stars in a relativistic model

Abstract

We study the entrainment effect between superfluid neutrons and charge neutral fluid (called the proton fluid) which is made of protons and electrons in neutron star interior within the two fluid formalism and using a relativistic model where baryon-baryon interaction is mediated by the exchange of $\sigma$, $\omega$ and $\rho$ mesons. This model of strong interaction also includes scalar self interactions. The entrainment matrix and entrainment parameter are calculated using the parameter sets of Glendenning (GL) and another non-linear (NL3) interaction. The inclusion of $\rho$ mesons strongly influences the entrainment parameter (${\epsilon }_{mom}$) in a superfluid neutron star. The entrainment parameter is constant at the core and drops rapidly at the surface. It takes values within the physical range.

26 pages, 9 figures; revised version with new results and figures

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Cited by in corpus (8)

• Superfluidity and Superconductivity in Neutron Stars
• Numerical models for stationary superfluid neutron stars in general relativity with realistic equations of state
• Relativistic tidal properties of superfluid neutron stars
• The I-Love-Q Relations for Superfluid Neutron Stars
• Entrainment effects in neutron-proton mixtures within the nuclear-energy density functional theory. I. Low-temperature limit
• Force on a neutron quantised vortex pinned to proton fluxoids in the superfluid core of cold neutron stars
• Effect of superfluid matter of neutron star on the tidal deformability
• Slowly rotating superfluid neutron stars with isospin dependent entrainment in a two-fluid model