Role of f(T) gravity on the evolution of collapsing stellar model

The aim of this paper is to exhibit the instability epochs of self-gravitating objects coupled with anisotropic radiative matter content. We perform our analysis in the background of f(T) gravity which is the extended version of teleparallel gravity. We probe the instability regions by taking a peculiar model f(T)=T+αT2. We explore the basic equations in order to model stellar interior, including field, dynamical and junction equations. We then study linear perturbations of our system. We formulate the modified collapse equation by using Harrison-Wheeler equation of state. We develop the instability constraints at Newtonian and post-Newtonian regimes. The major outcome of our work reveals that the stiffness parameter plays a significant role in the stability of relativistic anisotropic stellar interior in f(T) gravity.