A generalized interacting Tsallis holographic dark energy model and its thermodynamic implications

Abstract

The present paper deals with a theoretical model for interacting Tsallis holographic dark energy (THDE) whose infrared cut-off scale is set by the Hubble length. The interaction Q between the dark sectors (dark energy and pressureless dark matter) of the universe has been assumed to be non-gravitational in nature. The functional form of Q is chosen in such a way that it reproduces well known and most used interactions as special cases. We then study the nature of the THDE density parameter, the equation of state parameter, the deceleration parameter and the jerk parameter for this interacting THDE model. Our study shows that the universe exhibits the usual thermal history, namely the successive sequence of radiation, dark matter and dark energy epochs, before resulting in a complete dark energy domination in the far future. It is shown the evolution of the Hubble parameter for our model and compared that with the latest Hubble parameter data. Finally, we also investigate both the stability and thermodynamic nature of this model in the present context.

Dynamical analysis and statefinder of Barrow holographic dark energy

“…: V,-vol HDE models is IR cutoff, different IR cutoffs can also result in new HDE models [10,12,60]. These new proposed HDE models were studied in various scenario [60][61][62][63][64][65][66][67][68][69][70][71][72][73][74][75].…”

Cosmic Consequences of Kaniadakis and Generalized Tsallis Holographic Dark Energy Models in the Fractal Universe

“…The parameter q is one which decides whether the universe is facing accelerated expansion or not (i.e., q < 0 gives the accelerated expansion of the universe while q > 0 when the universe has decelerating expansion behavior) [56,57]. The equation of state (EoS) parameter ω d is one which decides the phases of the cosmos (i.e., ω d < −1 represents the phantom phase of the universe, and −1 < ω d < −1/3 describes the quintessence phase while ω d > −1/3 gives the vacuum phase of the universe) [58,59]. The squared speed of sound C 2 s is another important cosmological parameter which decides whether the model is stable or not (i.e., C 2 s > 0 describes the stable model while C 2 s < 0 only when the model is unstable) [57,58,60].…”

“…The equation of state (EoS) parameter ω d is one which decides the phases of the cosmos (i.e., ω d < −1 represents the phantom phase of the universe, and −1 < ω d < −1/3 describes the quintessence phase while ω d > −1/3 gives the vacuum phase of the universe) [58,59]. The squared speed of sound C 2 s is another important cosmological parameter which decides whether the model is stable or not (i.e., C 2 s > 0 describes the stable model while C 2 s < 0 only when the model is unstable) [57,58,60]. The ratio of Ω m = ρ m /ρ c and Ω d = ρ d /ρ c called the coincidence parameter given byr = Ω m /Ω d = ρ m /ρ d decides the dark energy-and dark matter-dominated eras of the universe (i.e., 0 < Ω m /Ω d < 1 describes the dark energydominated era, and Ω m /Ω d > 1 gives the dark matterdominated era) [61].…”

Interacting Rényi Holographic Dark Energy in the Brans-Dicke Theory

“…Therefore, the interaction between DE and DM must be handled seriously. Then again, there exist limits for the quality of this association for different setups [34][35][36][37][38][39][40][41][42][43][44][45][46][47][48]. This newly proposed Rényi HDE has also been examined by many researchers by considering the interaction between DE and DM to explain the accelerated expansion of the Universe with different IR cut-offs in general relativity, braneworld, loop quantum cosmology, and modified gravity [49][50][51][52].…”

“…It is important to mention here that it seems there is a deep connection between quantum gravity and generalized entropy scenarios, and indeed, quantum aspects of gravity may also be considered as another motivation for considering generalized entropies[22,80]. Tsallis entropy is one of the generalized entropy measures which lead to acceptable results in the gravitational and different cosmological setups[23,25,43,[81][82][83][84][85][86][87][88][89]. Usually, Tsallis entropy is defined as[86]…”