English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

This paper analyzes the anisotropic stellar evolution governed by apolytropic equation of state in the framework of $f(R,T,Q)$ gravity, where$Q=R_{ab}T^{ab}$. We construct the field equations, hydrostatic equilibriumequation and trace equation to obtain their solutions numerically under theinfluence of $\sigma R^{2}+\gamma Q$ gravity model, where $\sigma$ and $\gamma$are arbitrary constants. We examine the dependence of various physicalcharacteristics such as radial/tangential pressure, energy density, anisotropicfactor, total mass and surface redshift for specific values of the modelparameters. The physical acceptability of the considered model is discussed byverifying the validity of energy conditions, causality condition, and adiabaticindex. We also study the effects arising due to the strong non-minimalmatter-curvature coupling on anisotropic polytropes. It is found that thepolytropic stars are stable and their maximum mass point lies within therequired observational Chandrasekhar limit.

Role of $\sigma R^{2}+\gamma R_{\mu\nu}T^{\mu\nu}$ Model on Anisotropic Polytropes