routinely, which is adopted here also, is to relate pressure and energy density by a linear expression [7]. For special choices of parameters we obtain islands of stability for such wormholes. To this end, we make use of numerical computation and plotting since the problem involves highly intricate functions for an analytical treatment. The action of EMGB gravity in 5D (without cosmological constant, i.e. Λ = 0) is in which κ is related to the 5D Newton constant and α is the GB parameter. Beside the Maxwell Lagrangian the GB Lagrangian L GB consists of the quadratic scalar invariants in the combination in which R =scalar curvature, R$_{µν}$ =Ricci tensor and R$_{µνρσ}$ =Riemann tensor. Variational principle of S with respect to g$_{µν}$ yields where the Lovelock ( H$_{µν}$ ) and Maxwell ( T$_{µν}$ ) tensors respectively are The Einstein tensor G$_{µν}$ is to be found from our metric ansatz S = κ ∫ √ | g | d $^{5}$x ( R + α L GB − 1 4 F$_{µν}$F µν ) (1) L GB = R 2 − 4 R$_{µν}$R µν + R$_{µνρσ}$R µνρσ (2) G$_{µν}$ + 2 αH$_{µν}$ = κ $^{2}$T$_{µν}$ (3) H$_{µν}$ = 2( − R σκτ µ R$_{νσκτ}$ − 2 R $_{µρνσ}$R ρσ − 2 R$_{µσ}$R σ ν + RR$_{µν}$ ) − 1 2 g$_{µν}$L$_{GB}$, (4) T$_{µν}$ = F$_{µα}$F α ν − 1 4 g$_{µν}$F$_{αβ}$F $^{αβ}$. (5) ds 2 = − f ( r ) dt 2 + dr 2 f ( r ) + r $^{2}$( dθ 2 + sin $^{2}$θ ( dφ 2 + sin $^{2}$φdψ $^{2}$)) , (6) 3 II. A BRIEF REVIEW OF 5D EMGB THIN-SHELLS The paper is organized as follows. In Sec. II the 5D EMGB thin-shell wormhole formalism has been reviewed briefly. We perturb the wormhole through radial linear perturbation and cast the problem into a potential-well problem in Sec. III. In Sec. IV we impose constraint conditions on parameters to determine possible stable regions through numerical analysis. The paper ends with Conclusion which appears in Sec. V.