Abstract
Dynamical analysis of spherically symmetric collapsing star surrounding in locally anisotropic environment with expansion-free condition is presented in $f(R,T)$ gravity, where $R$ corresponds to Ricci scalar and $T$ stands for the trace of energy momentum tensor. The modified field equations and evolution equations are reconstructed in the framework of $f(R,T)$ gravty. In order to acquire the collapse equation we implement the perturbation on all matter variables and dark source components comprising the viable $f(R,T)$ model. The instability range is described in Newtonian and post-Newtonian eras by constraining the adiabatic index $\Gamma$ to maintain viability of considered model and stable stellar configuration.
Highlights
The astrophysics and astronomical theories are invigorated largely by the gravitational collapse and instability range explorations of self-gravitating objects
The mysterious content named dark energy (DE), occupying the major part of the universe is significant in the description of cosmic speed-up
The modified gravity theories are assumed to be effective in understanding the cosmic acceleration by induction of the so-called dark matter components in the form of higher order curvature invariants
Summary
The astrophysics and astronomical theories are invigorated largely by the gravitational collapse and instability range explorations of self-gravitating objects. Celestial objects tend to collapse when they exhaust all their nuclear fuel, and gravity takes over as the inward governing force. The gravitating objects are interesting only when they are stable against fluctuations; supermassive stars tend to be more unstable in comparison to the less massive stars [5]. The instability problem in a star’s evolution is of fundamental importance; Chandrasekhar [6] presented the primary explorations on the dynamical instability of spherical stars. He identified the instability range of a star having mass
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