Viable and Stable Compact Stellar Structures in f(Q,T)$f(\mathcal {Q},\mathcal {T})$ Theory

• Published in: Fortschritte der Physik 2024-03, Vol.72 (3), p.n/a
• Main Authors: Gul, M. Zeeshan, Sharif, M., Arooj, Adeeba
• Format: Article
• Language: English
• Subjects: Anisotropy; Astronomical models; compact objects; Equations of state; f(Q,T)$f(\mathcal {Q},\mathcal {T})$ theory; matching conditions; Parameters; Red shift; Stellar models; Tensors
• ISSN: 0015-8208; 1521-3978
• DOI: 10.1002/prop.202300221

The main objective of this paper is to investigate the impact of f(Q,T)$f(\mathcal {Q},\mathcal {T})$ gravity on the geometry of anisotropic compact stellar objects, where Q$\mathcal {Q}$ is non‐metricity and T$\mathcal {T}$ is the trace of the energy‐momentum tensor. In this perspective, the physically viable non‐singular solutions to examine the configuration of static spherically symmetric structures is used. A specific model of this theory to examine various physical quantities in the interior of the proposed compact stars (CSs) is considered. These quantities include fluid parameters, anisotropy, energy constraints, equation of state parameters, mass, compactness, and redshift. The Tolman–Oppenheimer–Volkoff equation is used to examine the equilibrium state of stellar models, while the stability of the proposed CSs is investigated through sound speed and adiabatic index methods. It is found that the proposed CSs are viable and stable in the context of this theory. The main objective of this paper is to investigate the impact of f(Q,T)$f( {\mathcal{Q},\mathcal{T}} )$ gravity on the geometry of anisotropic compact stellar objects, where Q$\mathcal{Q}$ is non‐metricity and T$\mathcal{T}$ is the trace of the energy‐momentum tensor. In this perspective, the physically viable non‐singular solutions to examine the configuration of static spherically symmetric structures is used. A specific model of this theory to examine various physical quantities in the interior of the proposed compact stars (CSs) is considered. These quantities include fluid parameters, anisotropy, energy constraints, equation of state parameters, mass, compactness, and redshift. The Tolman–Oppenheimer–Volkoff equation is used to examine the equilibrium state of stellar models, while the stability of the proposed CSs is investigated through sound speed and adiabatic index methods. It is found that the proposed CSs are viable and stable in the context of this theory.