Abstract
The aim of this paper is to investigate the stable/unstable regimes of the non-static anisotropic filamentary stellar models in the framework of f(R,T,R_{mu nu }T^{mu nu }) gravity. We construct the field equations and conservation laws in the perspective of this model of gravity. The perturbation scheme is applied to the analysis of the behavior of a particular f(R,T,R_{mu nu }T^{mu nu }) cosmological model on the evolution of cylindrical system. The role of the adiabatic index is also checked in the formulations of the instability regions. We have explored the instability constraints in the Newtonian and post-Newtonian limits. Our results reinforce the significance of the adiabatic index and dark source terms in the stability analysis of celestial objects in modified gravity.
Highlights
The accelerated expansion of the cosmos has become clearly manifest after the discovery of unexpected reduction in the detected energy fluxes coming from supernovae of type Ia [1,2]
We examined that adiabatic index 1 has significant role in the dynamical instability of these massive stars [37]
The dynamical equations are developed by using the contraction of the Bianchi identities
Summary
The accelerated expansion of the cosmos has become clearly manifest after the discovery of unexpected reduction in the detected energy fluxes coming from supernovae of type Ia [1,2]. Sharif and Manzoor [35] studied the dynamical instability of the axially symmetric stellar structure with reflection degrees of freedom coupled with locally anisotropic fluid configurations in self-interacting Brans– Dicke gravity and obtained stability conditions through the adiabatic index in both the N and the pN approximations. We have investigated the anisotropic spherical collapse in the background of f (R, T, Q) gravity and discussed the stability of compact stars by taking into account the particular viable model with perturbation technique. 2. Section 3 deals with the dynamics of cylindrical self-gravitating collapsing model in which formation of field equations and conservation laws by linear perturbation technique and instability constraints at Newtonian (N) and post-Newtonian (pN) limits are investigated.
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