Relativistic tidal properties of superfluid neutron stars

TL;DR

This paper models the tidal deformability of superfluid neutron stars using a relativistic two-fluid approach with entrainment, providing insights into their structure and response to gravitational tides.

Contribution

It introduces a relativistic two-fluid formalism with entrainment effects to analyze the tidal properties of superfluid neutron stars.

Findings

Calculated the equilibrium structure of superfluid neutron stars.

Determined the electric-type Love number for these stars.

Used a relativistic mean field model for the equation of state.

Abstract

We investigate the tidal deformability of a superfluid neutron star. We calculate the equilibrium structure in the general relativistic two-fluid formalism with entrainment effect where we take neutron superfluid as one fluid and the other fluid is comprised of protons and electrons, making it a charge neutral fluid. We use a relativistic mean field model for the equation of state of matter where the interaction between baryons is mediated by the exchange $\sigma$, $\omega$ and $\rho$ mesons. Then, we study the linear, static $l=2$ perturbation on the star to compute the electric-type Love number following Hinderer's prescription.