Diagnosing interacting Tsallis holographic dark energy in the non-flat universe

Abstract

This paper explores the interacting Tsallis holographic dark energy (THDE) model in a non-flat universe following an infrared cutoff as the apparent horizon. The equation of state (EoS) and the deceleration parameter of THDE model are determined to understand the cosmological evolution for interacting THDE model in the non-flat universe. By applying the statefinder [Formula: see text] parameter-pairs diagnostic and [Formula: see text] pair dynamical analysis for the derived THDE model, we plot the evolutionary trajectories for different cases of Tsallis parameter [Formula: see text] and interaction term [Formula: see text] and also, for spatial curvature [Formula: see text], [Formula: see text] and [Formula: see text] corresponding to flat, open and closed universes, respectively, in the framework of Planck 2018 base cosmology results VI-LCDM observational data.

Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

“…They also obtained the HDE from the fluid/gravity duality constraint through cosmological observations. Sharma et al [33] calculated the EoS and the deceleration parameter of the Tsallis HDE model to understand cosmological evolution by exploring the interacting Tsallis HDE model in a non-flat universe, with an infrared cut-off as the apparent horizon. By choosing the relationship between interacting dark matter and different HDE fluid environment models, Shekh and Ghaderi [34] have developed a Hypersurface-homogeneous cosmological model of the universe with interacting dark matter and other HDE fluid environment models.…”

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

“…As the universe evolves to the present time, the position of the curves with negative and positive spatial curvature changes and at the late times, the THDE density parameter for k > 0 dominates the case with k < 0 and the flat one. It is therefore reasonable to examine the results of present study by following the methods as presented in [108][109][110]. This also helps us to find out possible differences between flat and non-flat cases in a more concrete way.…”

“…Therefore, we conclude that for the deep understanding of behavior of interacting THDE, more investigations should be done. In this context, it deserves to mention here that Sharma et al [108] recently explored an interacting THDE model (with b 2 1 = b 2 2 = b 2 ) in the framework of a non-flat universe and also by considering apparent horizon as IR cutoff from the statefinder and ω D − ω D pair viewpoint. They showed the evolution of q, for different Tsallis parameter δ and b 2 and also distinct spatial curvature contributions corresponding to the flat, closed and open universes, respectively.…”

Reply to Pessoa, P.; Arderucio Costa, B. Comment on “Tsallis, C. Black Hole Entropy: A Closer Look. Entropy 2020, 22, 17”

“…Neither in [ 2 ] nor in [ 3 ] is a specific position taken for black holes being or physical objects, or even (multi)fractal objects with nonintenger d (which, to the best of our knowledge, may not be excluded). At the present stage, it seems appropriate to analyze this nontrivial and delicate issue within the specialized realm of cosmological and black-hole physics [ 4 , 5 , 6 , 7 , 8 , 9 , 10 , 11 , 12 , 13 , 14 , 15 , 16 , 17 , 18 , 19 , 20 , 21 , 22 , 23 , 24 , 25 , 26 , 27 , 28 , 29 , 30 , 31 , 32 , 33 , 34 , 35 , 36 , 37 , 38 , 39 , 40 , 41 , 42 , 43 , 44 , 45 , 46 , 47 , 48 ]. However, it is seemingly undeniable that the sort of perplexity expressed in [ 49 , …”