Strange Quark Stars and Condensate Dark Stars in Bumblebee Gravity

TL;DR

This study explores how Bumblebee gravity, involving spontaneous Lorentz symmetry breaking, affects the structure and properties of relativistic dark and strange quark stars, providing new bounds based on observational data.

Contribution

It introduces a detailed analysis of relativistic star models within Bumblebee gravity, incorporating analytic equations-of-state for dark and strange quark stars, and derives observational bounds on the theory.

Findings

Bumblebee parameter $ extbf{l}$ influences star structure significantly.

Mass-radius relations are computed for different star types.

Upper bounds on $ extbf{l}$ are established using pulsar and compact object data.

Abstract

In this paper, we investigate the properties of relativistic stars made of isotropic matter within the framework of the minimal Standard Model Extension, where a Bumblebee field (BF) coupled to spacetime induces spontaneous Lorentz symmetry breaking. We adopt analytic equations-of-state describing either condensate dark stars or strange quark stars. We solve the structure equations numerically, and we compute the mass-to-radius relationships. The influence of the Bumblebee parameter $\mathbf{l}$ is examined in detail, and an upper bound is obtained using the massive pulsar (PSR) J0740+6620 and the strangely light High Energy Stereoscopic System (HESS) J1731-347 compact object.