Study of viable compact stellar structures in non-Riemannian geometry

Abstract

The main objective of this article is to investigate the viable
compact stellar structures in non-Riemannian geometry, i.e.,
$f(\mathbb{Q},\mathbb{T})$ theory, where $\mathbb{Q}$ defines the
non-metricity and $\mathbb{T}$ represents trace of the stress-energy
tensor. For this purpose, we consider a static spherical spacetime
with anisotropic matter configuration to examine the geometry of
considered compact stars. A specific model of this theory is used to
derive the explicit expressions of energy density and pressure
components that govern the relationship between matter and geometry.
The unknown constants in the metric potentials are determined by
using the continuity of interior and exterior spacetimes to examine
the configuration of spherical stellar structures. Physical
parameters such as fluid characteristics, energy constraints and
equation of state parameters are analyzed to examine the viability
of the considered stellar objects. Further, the equilibrium state
and stability of the proposed stellar objects are evaluated using
the Tolman-Oppenheimer-Volkoff equation, sound speed and adiabatic
index, respectively. The rigorous analysis and satisfaction of
necessary conditions lead to the conclusion that the stellar objects
studied in this framework are viable and stable.