Global monopole induced wormholes in power-law gravity: stability and physical viability
Аннотация
Abstract In this manuscript, we examine geometrical and physical properties of wormhole ( $$\mathcal{W}\mathcal{H}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>W</mml:mi> <mml:mi>H</mml:mi> </mml:mrow> </mml:math> ) solutions with monopole charge by considering three distinct shape function models in power-law gravity, i.e., Starobinsky f ( R ) gravity, where R is Ricci scalr. The modified gravitational field equations are solved under the assumption of anisotropic energy–momentum tensor ( $$\mathcal {EMT}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>EMT</mml:mi> </mml:math> ), with particular attention given to the role of exotic matter ( $$\mathcal{E}\mathcal{M}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>E</mml:mi> <mml:mi>M</mml:mi> </mml:mrow> </mml:math> ) in sustaining these solutions. The impact of the global monopole charge ( $$\mathcal {GMC}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>GMC</mml:mi> </mml:math> ) is examined in detail, revealing that higher monopole charges enlarge the throat radius and produce flatter embedding surfaces through two and three dimensional embedding diagrams, thereby affecting both traversability and structural stability. A comprehensive investigation of physical quantities, energy conditions and stability analysis is carried out using several physical and geometrical criteria, including the adiabatic index approach, Herrera’s cracking criterion, and causality conditions approach, along with anisotropic effects. Moreover, the total amount of $$\mathcal{E}\mathcal{M}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>E</mml:mi> <mml:mi>M</mml:mi> </mml:mrow> </mml:math> is quantified through the volume integral quantifier method. These findings highlight supportive directions for future explorations of exotic spacetime structures in both theoretical and astrophysical contexts.