Noncommutative geometry, an offshoot of string theory, replaces pointlike structures with smeared objects and has recently been extended to higher dimensions. The purpose of this paper is to obtain wormhole solutions with this extended noncommutative geometry as a background. It is found through this investigation that wormhole solutions exist in the usual four, as well as in five dimensions, but they do not exist in higher-dimensional spacetimes.

This is a continuation and generalization of our earlier work on gravastar in (2+1) anti-de Sitter space–time to (2+1)-dimensional solution of charged gravastar. Morphologically this gravastar contains three regions, namely: (i) charged interior, (ii) charged shell and (iii) electrovacuum exterior. We have studied different characteristics in terms of Length and Energy, Entropy, and Junction conditions of the spherical charged distribution. It is shown that the present model of charged gravastar is non-singular and represents itself an alternative of black hole

This study examines the structure and stability of dark energy stars within the context of $$R^2$$ R 2 gravity, with the gravity model defined by $$f(R) = R + a R^2$$ f ( R ) = R + a R 2 (the Starobinsky model). Specifically, dark energy is a mysterious force that can prevent the gravitational collapse of compact objects to singularities. To characterize dark energy, we consider modified Chaplygin fluid as an equation of state (EoS) of matter and study its mass-radius relation for different model parameters. By numerically solving the modified Tolman–Oppenheimer–Volkoff (TOV) equations, our primary objective is to examine the influence of variations in the $$R^2$$ R 2 gravity parameter a on the energy density, pressure, mass-radius and mass-central density relationships of dark energy stars. Our findings reveal that the variation of a does not significantly impact on the $$(M-R)$$ ( M - R ) relations but comfortably exceeds the 2 $$M_{\odot }$$ M ⊙ limit. Additionally, we examine the dynamical stability of these stars by evaluating the static stability criterion, adiabatic index, and sound speed. Finally, we compare our results with various astrophysical observational data and discuss future observations that could validate the predictions of our model.