Abstract
In this work, we have studied the accretion of dark energies onto a Morris–Thorne wormhole. Previously, in ref. (González-Díaz, arXiv:hep-th/0607137 ), it was shown that for quintessence like dark energy, the mass of the wormhole decreases, and for phantom like dark energy, the mass of the wormhole increases. We have assumed two types of dark energy: the variable modified Chaplygin gas and the generalized cosmic Chaplygin gas. We have found the expression of the wormhole mass in both cases. We have found the mass of the wormhole at late universe and this is finite. For our choices of the parameters and the function $$B(a)$$ , these models generate only quintessence dark energy (not phantom) and so the wormhole mass decreases during the evolution of the universe. Next we have assumed the five kinds of parametrizations of well-known dark-energy models. These models generate both quintessence and phantom scenarios i.e., phantom crossing models. So if these dark energies accrete onto the wormhole, then for the quintessence stage, the wormhole mass decreases up to a certain value (a finite value) and then again increases to an infinite value for the phantom stage during whole evolution of the universe. That means that if the five kinds of DE accrete onto a wormhole, the mass of the wormhole decreases up to a certain finite value and then increases in the late stage of the evolution of the universe. We have also shown these results graphically.
Highlights
A wormhole is a feature of space that is essentially a ‘shortcut’ from one point in the universe to another point in the universe, allowing travel between them that is faster than it would take light to make the journey through normal space
The Euclidean wormholes arise in Euclidean quantum gravity; the Lorentzian wormholes [10] are static spherically symmetric solutions of Einstein’s general relativistic field equations [11]
In order to support such exotic wormhole geometries, the matter should violate the energy conditions, but the average null energy condition is satisfied in wormhole geometries [12,13,14]
Summary
A wormhole is a feature of space that is essentially a ‘shortcut’ from one point in the universe to another point in the universe, allowing travel between them that is faster than it would take light to make the journey through normal space. The accretion of phantom dark energy onto a Schwarzschild black hole was first modeled by Babichev et al [26,27]. Accretion of a phantom like variable modified Chaplygin gas onto Schwarzschild black hole was studied by Jamil [28] who showed that the mass of the black hole will decrease when accreting fluid violates the dominant energy condition and otherwise will increase. Madrid et al [50] studied the dark-energy accretion onto black holes and worm holes phenomena could lead to unexpected consequences, allowing even the avoidance of the considered singularities. Martín-Moruno et al [51] have considered a general formalism for the accretion of dark energy onto astronomical objects, black holes, and wormholes. We give some concluding remarks of the whole work
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