Scalar- and Vector Dark Matter Admixed Neutron Stars

TL;DR

This paper investigates how bosonic dark matter, modeled as scalar or vector fields, affects neutron star properties, including mass, radius, and tidal deformability, by constructing and analyzing mixed fermion-boson star models.

Contribution

It introduces the first combined models of fermion and vector boson fields in neutron stars, called fermion Proca stars, and explores their equilibrium solutions and observational implications.

Findings

Fermion Proca stars tend to be more massive and larger than fermion boson stars.

Dark matter cores decrease neutron star tidal deformability, while clouds increase it.

Self-interaction strength significantly influences mass and tidal properties.

Abstract

It is believed that dark matter (DM) could accumulate inside neutron stars and significantly change their masses, radii and tidal properties. We study what effect bosonic dark matter, modelled as a massive and self-interacting scalar or vector field, has on neutron stars. We derive equations to compute the tidal deformability of the full Einstein-Hilbert-Klein-Gordon system self-consistently, and probe the influence of the scalar field mass and self-interaction strength on the total mass and tidal properties of the combined system, called fermion boson stars (FBS). We are the first to combine Proca stars with neutron stars to mixed systems of fermions and a vector field in Einstein-Proca theory, which we name fermion Proca stars (FPS). We construct equilibrium solutions of FPS, compute their masses, radii and analyse them regarding their stability and higher modes. We find that FPS tend to be more massive and geometrically larger than FBS for equal boson masses and self-interaction strengths. Both FBS and FPS admit DM core and DM cloud solutions and we find that they can produce degenerate results. Core solutions compactify the neutron star component and lower their tidal deformability, cloud solutions have the inverse effect. Electromagnetic observations of certain cloud-like configurations would appear to violate the Buchdahl limit. The self-interaction strength is found to significantly affect both mass and tidal deformability. We discuss observational constraints and the connection to anomalous detections. We also show how models with an effective equation of state compare to the self-consistent solution of FBS and find the self-interaction strength where both solutions converge sufficiently.