Viable and Stable Compact Stellar Structures in f(Q,T) Theory

Viable and Stable Compact Stellar Structures in f(Q,T) Theory

18 Feb 2024 | M. Zeeshan Gul, M. Sharif, Adeeba Arooj
This paper investigates the impact of $f(Q, \mathcal{T})$ gravity on the geometry of anisotropic compact stellar objects, where $Q$ represents non-metricity and $\mathcal{T}$ is the trace of the energy-momentum tensor. The authors use physically viable non-singular solutions to examine the configuration of static spherically symmetric structures. They consider a specific model of this theory to analyze various physical quantities within the proposed compact stars, including fluid parameters, anisotropy, energy constraints, equation of state parameters, mass, compactness, and redshift. The Tolman-Oppenheimer-Volkoff equation is used to determine the equilibrium state of the stellar models, and the stability of the compact stars is assessed through sound speed and adiabatic index methods. The results indicate that the compact stars are viable and stable in the context of this theory. The paper also discusses the basic formulation of $f(Q, \mathcal{T})$ gravity, the field equations, and matching conditions, providing a comprehensive analysis of the physical characteristics and stability of compact stars.This paper investigates the impact of $f(Q, \mathcal{T})$ gravity on the geometry of anisotropic compact stellar objects, where $Q$ represents non-metricity and $\mathcal{T}$ is the trace of the energy-momentum tensor. The authors use physically viable non-singular solutions to examine the configuration of static spherically symmetric structures. They consider a specific model of this theory to analyze various physical quantities within the proposed compact stars, including fluid parameters, anisotropy, energy constraints, equation of state parameters, mass, compactness, and redshift. The Tolman-Oppenheimer-Volkoff equation is used to determine the equilibrium state of the stellar models, and the stability of the compact stars is assessed through sound speed and adiabatic index methods. The results indicate that the compact stars are viable and stable in the context of this theory. The paper also discusses the basic formulation of $f(Q, \mathcal{T})$ gravity, the field equations, and matching conditions, providing a comprehensive analysis of the physical characteristics and stability of compact stars.
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[slides] Viable and Stable Compact Stellar Structures in f(Q%2CT)%24f(%5Cmathcal %7BQ%7D%2C%5Cmathcal %7BT%7D)%24 Theory | StudySpace