Recently one and two-parameter deformed Einstein equations have been studied for extremal quantum black holes which have been proposed to obey deformed statistics by Strominger. In this study, we give a deeper insight to the deformed Einstein equations and consider the solutions of these equations for the extremal quantum black holes. We then represent the implications of the solutions, such that the deformation parameters lead the charged black holes to have a smaller mass than the usual Reissner-Nordström black holes. This reduction in mass of a usual black hole can be considered as a transition from classical to quantum black hole regime.
We consider a novel dark energy model to investigate whether it will provide an expanding universe phase. Here we propose a mixed dark energy domination which is constituted by a tachyon, quintessence and phantom scalar fields non-minimally coupled to gravity, in the absence of background dark matter and baryonic matter, in the framework of teleparallel gravity. We perform the phase-space analysis of the model by numerical methods and find the late-time accelerated attractor solutions implying the acceleration phase of universe.2 energy constitution are quintessence, phantom and tachyon fields. We can briefly classify the dark energy models in terms of the most powerful quantity of dark energy; its equation of state parameter DE DE DE p / , where DE p and DE are the pressure and energy density of the dark energy, respectively. For cosmological constant boundary 1 DE , but for quintessence the parameter 1 DE , for phantom 1 DE and for non-minimally coupled tachyon with gravity both 1 DE and 1 DE [16-18]. The scenario ofDE crosses the cosmological constant boundary is referred as a "Quintom" scenario. The explicit construction of Quintom scenario has a difficulty, due to a no-go theorem. The equation of state parameter DE of a scalar field cannot cross the cosmological constant boundary according to no-go theorem, if the dark energy described by the scalar field is minimally coupled to gravity in Friedmann-Robertson-Walker (FRW)geometry. The requirement for crossing the cosmological constant boundary is that the dark energy should non-minimally coupled to gravity, namely it should interact with the gravity [19][20][21][22][23][24]. There are also models in which possible coupling between dark energy and dark matter can occur [25,26]. In this paper, we consider a mixed dark energy model constituted by a tachyon, quintessence and phantom scalar fields non-minimally coupled to gravity.The mixed dark energy model in this study is considered in the framework of teleparallel gravity instead of classical gravity. The teleparallel gravity is the equivalent form of the classical gravity, but in place of torsion-less Levi-Civita connection, curvature-less
We propose a novel coupled dark energy model which is assumed to occur as a qdeformed scalar field and investigate whether it will provide an expanding universe phase. We consider the q-deformed dark energy as coupled to dark matter inhomogeneities. We perform the phase-space analysis of the model by numerical methods and find the late-time accelerated attractor solutions. The attractor solutions imply that the coupled q-deformed dark energy model is consistent with the conventional dark energy models satisfying an acceleration phase of universe. At the end, we compare the cosmological parameters of deformed and standard dark energy models and interpret the implications.
Recently q-deformed Einstein equations have been studied for extremal quantum black holes which have been proposed to obey deformed statistics by Strominger. In this study, we give the solutions of deformed Einstein equations by considering these equations for the charged black holes. Also we present the implications of the solutions, such as the deformation parameters lead the charged black holes to have a smaller mass than the classical Reissner-Nordström black holes. The reduction in mass of a classical black hole can be viewed as a transition from classical to quantum black hole regime.
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