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 is devoted to discuss compact stars in$f(\mathscr{R},\mathscr{G})$ gravity, where $\mathscr{R}$ and $\mathscr{G}$denote the Ricci scalar and Gauss-Bonnet invariant respectively. To meet thisaim, we consider spherically symmetric space-time with anisotropic fluiddistribution. In particular, the Karmarkar condition is used to explore thecompact star solutions. Further, we choose two specific model of compact starsnamely LMC X-4 (mass =1.29$M/M_{\odot}$ \& radii=9.711 km) and EXO 1785-248(mass =1.30$M/M_{\odot}$ \& radii=8.849 km). We develop the field equations for$f(\mathscr{R},\mathscr{G})$ gravity by employing the Karmarkar condition witha specific model already reported in literature by Lake [Phys. Rev. D 67,104015 (2003)]. We further consider the Schwarzschild geometry for matchingconditions at the boundary. It is important to mention here that we calculatethe values of all the involved parameter by imposing the matching condition. Wehave provided a detailed graphical analysis to discuss the physicalacceptability of parameters, i.e., energy density, pressure, anisotropy, andgradients. We have also examined the stability of compacts stars by exploringthe energy conditions, equation of state, generalizedTolman-Oppenheimer-Volkoff equation, causality condition, and adiabatic index.For present analysis, we predict some numerical values in tabular form forcentral gravitational metric functions, central density and central pressurescomponents. We have also calculated the ratio $p_{rc}/ \rho_{c}$ to check thevalidity of Zeldovich's condition. Conclusively, it is found that our obtainedsolutions are physically viable with well-behaved nature in$f(\mathscr{R},\mathscr{G})$ modified gravity for the compact star models underdiscussion.

Physically viable solutions of anisotropic spheres in $f(\mathscr{R},\mathscr{G})$ gravity satisfying the Karmarkar condition