Influence of modification of gravity on the dynamics of radiating spherical fluids

Abstract

We explore the evolutionary behaviors of compact objects in a modified gravitational theory with the help of structure scalars. Particularly, we consider the spherical geometry coupled with heat and radiation emitting shearing viscous matter configurations. We construct structure scalars by splitting the Riemann tensor orthogonally in f (R, T ) gravity with and without constant R and T constraints, where R is the Ricci scalar and T is the trace of the energy-momentum tensor. We investigate the influence of modification of gravity on the physical meaning of scalar functions for radiating spherical matter configurations. It is explicitly demonstrated that even in modified gravity, the evolutionary phases of relativistic stellar systems can be analyzed through the set of modified scalar functions.

Energy conditions in modified f(G) gravity

“…For simplicity, we let α = 1, β = 1 and plot ρ eff and ρ eff + p eff which are the function of m and n only, as shown in fig.3. It can be observed from this figure that WEC is also valid for the model (19). Now, we will check the constraints on parameters for the validity of WEC.…”

“…To get an exact solution from the above two inequalities (17) and (18), for the parameters α, β and n, is a quite hard task. In order to achieve this goal, we would consider specific value of α = 0.3 and plot ρ eff and ρ eff + p eff as a function of β and n as shown in fig.1.…”

“…The concept of modified gravity theories (MGTs) obtained by replacing the Ricci scalar in the standard Einstein-Hilbert (EH) action with some generic functions of the Ricci scalar f (R) or the combinations of the scalar and tensorial curvature invariants have been introduced by many relativistic astrophysicists. This approach has now been referred as a standard terminology whose formulations could be considered as a viable guide to explore reason of the cosmic accelerated expansion (for further reviews on dark energy and modified gravity, see, for instance, [10][11][12][13][14][15][16][17][18][19][20][21][22][23][24]). The first consistent outcomes of accelerating universe from f (R) gravity was suggested by Nojiri and Odintsov [25].…”

Role of $$f(R,T,R_{\mu \nu }T^{\mu \nu })$$ f ( R , T , R μ ν T μ ν ) model on the stability of cylindrical stellar model

“…Cembranos et al [19] studied gravitational collapse in f (R) gravity and found this phenomenon to possibly work as a key tool to constrain modified gravity models that describe late time cosmological acceleration. Yousaf et al [20,21] investigated the irregularity constituents for spherical selfgravitating stars in the presence of an imperfect matter distribution within f (R, T ) gravity and found that the complexity of matter increases with the increase of anisotropic stresses. Yousaf [22] explored collapsing spherical models supporting a vacuum core in a -dominated era within the stellar interior.…”

Role of tilted congruence and f(R) gravity on regular compact objects

“…Bhatti and his coworkers [21] examined the impact of extra Ricci curvature terms on the stability of spherical compact objects filled with anisotropic relativistic matter distributions. Yousaf et al [22] explored the contribution of f (R, T ) extra curvature terms in the outcomes of inhomogeneity factors for dissipative spherical system. They also found factors that causes the maintenance of homogeneous or inhomogeneous matter state, when the system departs hydrostatic equilibrium phase in modified gravity [23].…”