Weak gravitational lensing by black holes and wormholes in the context of massive gravity (Bebronne and Tinyakov, JHEP 0904:100, 2009) theory is studied. The particular solution examined is...

A new solution satisfying the Karmarkar condition is presented here. We were first to have discovered a hypergeometric function metric potential representing embedding class I spacetime. This new...

We present a new traversable wormhole explication of Einstein’s field equations supported by the profile of Einasto Dark Matter densities (Einasto in Trudy Inst Astrofiz Alma-Ata 51:87, 1965; PTarO 36:414, 1968; Astron Nachr 291:97, 1969) and global monopole charges along with semiclassical effects in the local universe as the galactic halo. The Einasto DM density profile produces a suitable shape function that meets all the requirements for presenting the wormhole geometries. The Null Energy Condition (NEC) is violated by the obtained solution with different redshift functions i.e. the Einasto profile representing DM candidate within the wormholes gives the fuel to sustain these wormhole structures in the galactic halo. Moreover, the reported wormhole geometries are getting asymptotically flat and non-flat depending only on the choices of redshift function whereas all the wormhole structures are maintaining their balance of equilibrium under the action of different forces.

In this article, we are proposing a model of anisotropic compact star possessing density profile of pseudo-isothermal dark matter satisfying a linear equation of state (EoS). The stellar system supported by this density profile is physically possible and in equilibrium fulfilling all the energy conditions including the TOV-equation. The solution also satisfies the causality condition, static stability criterion, Abreu’s stability and Bondi’s criteria. The fulfillment of Rhoades–Ruffini criterion makes our solution more physically viable as well. The M–R curve is plotted for $$b=12.55$$b=12.55 km and $$B_g=60$$Bg=60 MeV/fm $$^3$$3 .

The present work looks for the existence of completely new wormhole geometries in the bulge of the Milky Way galaxy (MWG) situated on the dark matter (DM) density profile followed from MacMillan (MNRAS 76:465, 2017) and Boshkayev and Malafarina (MNRAS 484:3325, 2019) concerned with Global Monopole Charge. The obtained shape function is positively increasing against the radial coordinate and it increases faster with the increasing values of Global Monopole Charge. Moreover, the reported shape function satisfies all the essential criterions and hence it constructs wormhole geometry in the bulge of the MWG. Further, the DM candidate around bulge is suitable to harbor wormhole by violating the null energy condition(NEC) corresponding to three different redshift functions. The striking point of our solution is that for zero Global Monopole Charge the wormholes are asymptotically flat corresponding to the first two choices of redshift functions while for positive values of Global Monopole Charge wormhole becomes non asymptotically flat and Global Monopole Charge also has the crucial effect on the violation of NEC. In our solutions, one can note that the total amount of averaged NEC violating matter in the wormhole spacetime depends on the Global Monopole Charge $$\eta $$η . Furthermore, the respective wormhole solutions are in equilibrium positions.

In this article, we present a new model for anisotropic compact stars confined to physical dark matter (DM) based on the Bose–Einstein DM density profile and a bag model type equation of state (EoS). The obtained solutions are physically well-behaved and represent the physical and stable matter configuration by satisfying the energy conditions, causality conditions, and essential conditions on the stability factor and adiabatic index. The solutions supporting the matter sphere are in an equilibrium state by satisfying the generalized TOV equation. We also find the surface redshift, compactness parameter at the surface, maximum mass, and interestingly, all these values are under the desired range that makes our solution more physically viable. Here, the radially symmetric profiles of energy density, radial and transverse pressures are demonstrated.