Rapidly rotating Dirac stars

TL;DR

This paper constructs and analyzes sequences of rapidly rotating Dirac stars within general relativity, revealing their stability domain and physical characteristics, which resemble those of rotating neutron stars under certain conditions.

Contribution

It introduces a new model of rotating Dirac stars using a spinor fluid with an effective equation of state, exploring their stability and physical properties.

Findings

Identified the stable configuration domain of rotating Dirac stars.

Calculated their principal characteristics based on central density, spinor field mass, and rotation velocity.

Found similarities between Dirac stars and rotating neutron stars for specific spinor field masses.

Abstract

Within general relativity, we construct sequences of rapidly rotating Dirac stars consisting of a spinor fluid described by an effective equation of state. We find the physically relevant domain of stable configurations and calculate their principal characteristics which are completely determined by the central density of the spinor fluid, the mass of the nonlinear spinor field, and the velocity of rotation. It is demonstrated that for a certain choice of the spinor field mass, the main physical characteristics of the Dirac stars are close to those that are typical of rotating neutron stars.