Abstract
The paper investigates the Tsallis holographic dark energy (THDE) model in accordance with the apparent horizon as an infrared cut  off, in a non flat universe. The cosmological evolution of the deceleration parameter and equation of state of THDE model are calculated. The evolutionary trajectories are plotted for the THDE model for distinct values of the Tsallis parameter besides distinct
spatial curvature contributions, in the statefinder parameterpairs and plane, considering the present value of dark energy density parameter
, , in the light of observational data.
The statefinder and plane plots
specify the feature of the THDE and demonstrate the separation
between this framework and other models of dark energy.
Keywords : Tsallis, Holographic, Statefinder, Dark energy
PACS: 98.80.Es, 95.36.+x, 98.80.Ck
Tsallis holographic model of dark energy: Cosmic behaviour, statefinder analysis and pair in the non flat universe
Vipin Chandra Dubey, Umesh Kumar Sharma, A. Beesham
Department of Mathematics, Institute of Applied Sciences and Humanities, GLA University
Mathura281 406, Uttar Pradesh, India
Department of Mathematical Sciences, University of Zululand, KwaDlangezwa 3886, South Africa
Email: vipin.dubey@gla.ac.in.
Email: sharma.umesh@gla.ac.in
Email: beeshama@unizulu.ac.za
1 Introduction
The dark area of the cosmos intrigues the scholars and the latest surveys
[1, 2, 3, 4, 5, 6, 7, 8, 9, 10], demonstrate that the dark sector contribution is in roughly in comparison to substratum ;
rest is negligible radiation and baryonic matter (about ). The baryonic matter comprises electromagnetic
radiation
and may be seen precisely [11]. The dark matter, which around of the
matter part of the universe is a pressure less matter, which gives
the velocity of galaxy clusters [12]. It was inferred that there was more mass in galaxies; than observed by the corroboration CDM with the examinations of rotational trajectories of spiral galaxies [13]. This exotic matter presence is affirmed by the gravitational lensing and galaxy clusters on the basis of xray emission.
The dark energy, around of the rest cosmic foundation, is responsible for the current accelerated stage of the universe [14, 15]. Under the standard cosmological description, the cosmological constant may be used for DE component, which is having a geometric nature in accordance with the GR with constant energy density and EoS (equation of state) [16, 17]. The description of dark energy is in toe with
recent observational data, but it opposes the theoretical
prediction for vacuum energy, which has been observed by quantum field theory [18]. This material description has the inflationary paradigm,
the Big Bang nucleosynthesis (BBN) and general relativity (GR), called the CDM model. Normally dynamical description is taken for DE part via a
distinct EoS, instead of the vacuum description, for example, EoS parameter (constant or timedependent) [19, 20]. Other proposed DE component are the
dynamical approach through a scalar field [21, 22] and modified theories of
gravity [23, 24, 25, 26].
Holographic dark enegy (HDE) is an interesting attempt to explain the current accelerated expansion of the universe [27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 42, 43, 44] in line with some observations [45, 46, 47, 48, 49], within the framework of holographic rule [50, 51, 52] by characterizing and portraying the established holographic energy density as , contingent upon the entropy connection of black holes [27], here c denotes constant. Such models are in incredible concurrence with ongoing observations and have drawn the consideration of scientists as of late. Also, a few
other holographic rule persuaded DE models have likewise been recommended [53, 54, 55].
Recently, various DE models being produced for deciphering or portraying the accelerated expansion of the universe, are accessible. With a specific genuine goal to be able to confine between these battling cosmological scenarios including DE, a delicate and exceptional feature for DE models is an absolute need. Thus, a logical suggestion that impacts the utilization of the determination of pair , the specified ”statefinder”, was suggested by Sahni et al. [56, 57]. It is not elusive that the statefinder parameters to refine the universe evolution components through the higherorder derivative of the scale factor (a) and is a trademark following stage past Hubble parameter () and deceleration parameter (). Since various cosmological models including DE demonstrate dynamically special advancement directions in the plane, consequently, statefinder is a helpful tool for seeing these DE models which are characterized as
(1) 
The geometrical analysis, statefinder is constructed directly from spacetime metric, as it is considered as universal, is basically modeldependent in describing the dark energy. To find the qualitatively different behaviours to that of models of dark energy, the plane is taken into consideration for plotting the evolutionary trajectories. The spatially flat CDM is defined by the fixed point i.e.
. The displacement of the derived model from CDM is calculated by the displacement from this fixed point to a dark energy model, which provides a good way of observing
this distance. As explored in
[57, 58, 59, 60, 61, 62, 63, 64, 65, 66, 67, 68, 69, 70, 71, 72] the statefinder may effectively differentiate between
a wide variety of dark energy models including quintessence, the cosmological
constant, braneworld and the Chaplygin gas models and
interacting dark energy models. Recently, Sharma
and Pradhan (2019) and Gunjan et al. (2019) have diagnosed
the geometric behaviour of noninteracting and
interacting THDE for a flat universe in terms of statefinder parameters and
pair in detail [73, 74]. Sheykhi (2018), have derived the modified Friedmann equations for an FRW universe with the apparent horizon as IR cutoff in the form of Tsallis entropy [75].
In this work, we apply the statefinder diagnosis and plane diagnostic to the THDE model
in the nonflat universe with the apparent horizon as IR cutoff. The statefinder may likewise be utilized to analyze distinctive illustration of the model, including different model parameters and distinctive spatial curvature () inputs.
Moreover, we consider the values of
, and
corresponding to the open, closed and flat universes, respectively, in the light of [6] and by
varying the Tsallis parameter [76, 77].
The sequence of the paper is as follows: In Sec. 2, we review the
THDE considering the IR cutoff as the apparent horizon. In Sec. 3, observational data is given. In Sec. 4, the cosmic behaviour of the deceleration parameter and EoS is described. In Sec. 5,
the statefinder parameters are obtained and plotted. In Subsec. 5.1, plane is explored. Discussions and Conclusions are talked about in Sec. 6
2 THDE : Brief review with IR cutoff as apparent horizon
The foundation of the HDE approach is the definition of the system boundary, and in fact, modification in the HDE models can be done by changing the system entropy [43, 44, 55, 78]. Additionally, statistical generalized mechanics produces a new entropy for black holes [76], an entropy which varies from the Bekenstein entropy and prompts another HDE model called THDE [77]. In [77], THDE has been investigated with Hubble horizon as IR cutoff which corresponds to the accelerated universe but was not stable. Recently, the THDE is investigated in different scenario with other IR cutoffs [79, 80, 81, 82, 83, 84, 85, 86]. Here, we have considered, the apparent horizon as IR cutoff as the usual system boundary for the FRW universe situated at [75, 87, 88, 89].
(2) 
Gibbs in 1902, pointed out that the standard BoltzmannGibbs theory is not suitable for divergent partition functions and largescale gravitational systems are in line this class. Also, it has been contended that frameworks including the longrange interactions may fulfil statistical generalized mechanics rather than the BoltzmannGibbs insights [83]. Tsallis [76] standard passes Gibbs theory as a limit. So, additive BoltzmannâGibbs entropy must be generalized to the nonextensive, i.e nonadditive entropy, which is called Tsallis entropy. The black hole horizon entropy can be modified as [76]
(3) 
where represents the nonadditive parameter and denotes unknown constant. Since a null hypersurface is represented by for the FRW spacetime and also, a proper system boundary [87, 88, 89], a property equivalent to that of the black hole horizon, one may observe as the IR cutoff, and utilize the holographic DE speculation to get [83, 86].
(4) 
where B denotes the unknown parameter. It was contended that the entropy related with the
apparent horizon of FRW universe, in every gravity hypothesis, has a similar structure as the same structure as the entropy of black hole horizon in the relating gravity. The
just change one need is supplanting the black hole horizon span by the apparent
horizon radius [83].
The metric for FRW nonflat universe is defined as :
(5) 
where , and represent a open, closed and flat universes, respectively. The first Friedmann equation in a nonflat FRW universe, including THDE and darkmatter (DM) is given as :
(6) 
where and represent the energy density of matter and THDE, respectively, and represent the ratio of energy densities of two dark sectors [43, 83]. Using the fractional energy densities, the energy density parameter of pressureless matter, THDE and curvature term can be expressed as
,
Now Eq. (6) can be written as:
(7) 
The law of conservation for matter THDE and are given as :
(8) 
(9) 
in which represents the THDE EoS parameter. Combining with the definition of , we get
(10) 
Now, using derivative with time of Eq. (6) in Eq. (9), and combined the result with Eqs. (8) and Eq. (7), we get
(11) 
Using Eq. (11), The deceleration parameter is obtained as
(12) 
Now, using the derivative with time of Eq. (4) with Eqs. (2) and Eq. (11), we get
(13) 
Now by using the time derivative of energy density parameter with Eqs. (13) and (11), one gets
(14) 
where, dot denotes derivative with respect to time, and prime denotes the derivative with respect to the ln a.
Additionally, calculations for the density parameter
(15) 
3 Observational Data
In this section, we introduce the observational data used in the analysis of Tsallis holographic dark energy model.
The streamlining presumptions of cosmic scale homogeneity and isotropy guide to the wellknown
FLRW metric that has all the earmarks of being an exact depiction of our universe. The base CDM cosmology expect a FLRW
metric with a flat 3space. This is a prohibitive presumption
that should be tried exactly. For FLRW models
compares to adversely bended 3geometries while
compares to emphatically bended 3geometries. Indeed, even with flawless information inside our past lightcone, our derivation of the curvature
is restricted by the cosmic variance of curvature perturbations
that are still superhorizon at the present since these can not be
recognized from background curvature inside our observable
volume.
The curvature parameter increases as a power law during the matter dominated and radiation era, but decreases exponentially with time during inflation, So the inflationary forecast has been that curvature ought to be imperceptibly small at present. By, adjusting parameters it is conceivable to
devise inflationary models that produce open [90, 91] or closed universes [92]. Indeed all the more theoretically, there has been intrigue as of late in multiverse models, in which topologically open ”pocket universes”
structure by bubble nucleation [93, 94] between various vacua of a ”string landscape” [95, 96]. Plainly, the recognition of a noteworthy deviation from would have significant ramifications for expansion hypothesis and Physics [7]. With primary CMB fluctuations alone [97, 98], the spatial curvature, , is constrained by the geometric degeneracy. Be that as it may, with the ongoing recognition of CMB lensing in the high power spectrum [99, 100], the degeneracy between
and is currently considerably decreased. This creates a huge identification of DE and tight limitations on spatial curvature utilizing just CMB information: when the ACT and SPT information, including the lensing limitations, are joined with nineyear WMAP information.
Bennett et.al [101], demonstrates the joint limitations on () (and , verifiably) from the as of now
accessible CMB information. Consolidating the CMB information with lowerredshift separate markers, such , BAO, or supernovae further constrains ([102]). Expecting the DE is vacuum energy (), it was given
WMAP+eCMB+BAO+.
The summary of the nonflat cosmological parameters used in this work is given in Table 1.
Parameter  WMAP + eCMB + BAO + 








4 Cosmological behaviour of the non  interactiing THDE model
and
(17) 
In order to describe cosmic evolution, we have obtained cosmological parameters, deceleration parameter and THDE EoS parameter which is given by Eqs. (16) and (17). In Fig. 1, we have plotted the evolutionary behaviour of the deceleration parameter versus redshift for different Tsallis model parameter and also different contributions of the spatial curvature. From this graph, the transition from decelerated to the accelerated universe occurs from closed, flat and open universes. Moreover, the difference between them is minor. our results show that the transition redshift from deceleration to accelerated phase lies in the interval , which is fully consistent with the observations [103].
The behaviour of THDE EoS parameter against redshift for THDE with the apparent horizon cutoff has been plotted in Fig. 2, for different Tsallis model parameter and also different contributions of the spatial curvature. From this figure, we may clearly see that the THDE model with the apparent cutoff can lead to accelerated expansion, and tends to at the future for closed, flat and open universes which implies that this model mimics the cosmological constant at late time.
5 Statefinder analysis for non  interacting THDE
Now, we discuss the statefinder analysis of the THDE
model. It ought to be referenced that the statefinder analysis with pair for THDE in the flat universe has been examined in detail in [73, 74], where the attention is put on the analysis of the various interims of parameter . In [73, 74], it has been exhibited that
from the statefinder perspective, assumes a key role. Here we need to concentrate on the statefinder analysis of the contributions of the spatial curvature. It is important that in the nonflat universe the CDM model does not compare a fixed point in the statefinder plane, it displays an evolution trajectory as
(18) 
The statefinder parameters and may also be expressed in terms of EoS parameter and energy density as follows [60] :
(19) 
(20) 
Note that the parameter
is also called cosmic jerk and , is the total energy density.
The statefinder parameter are obtained for THDE model as :
(21) 
(22) 
The first and second statefinder parameters against redshift have been plotted in Fig. 3 and 4. From these figures, we see that, both, first and second statefinder parameter at low redshift of THDE approaches that of CDM i.e. and , for different Tsallis model parameter and also open, flat and closed universes while
at large CDM deviates significantly from the standard behaviour. For Oscillating dark energy (ODE), the second statefinder parameter
at low redshift approaches that of CDM, while
at large CDM deviates significantly from the standard
behaviour. The opposite holds for the first parameter [68]. Cao et al [67], demonstrates the evolution of and versus redshift for theory. They have shown different features for these parameters. Cui and Zhang [104], compared the HDE, NHDE, RDE, NADE and CDM models with the first statefinder parameter and differentiate them in the lowshift region. Thus, the THDE models differ from ODE and other dark energy models in terms of the first and second statefinder parameter. It is of interest to see that the cases are distinctively differentiated in the low  redshift region.
We have plotted the evolution trajectories in the statefinder and
planes for our THDE model in Fig. 5 and Fig. 6, for different Tsallis parameter and also different contributions of the spatial curvature as
as 0.0027, 0 and 0.01
corresponding to the open, flat and closed universes, respectively. From Fig. 5, in evolutionary plane, we see that the derived THDE model, for open universe starts its evolutionary trajectories from , for , , for and , for , for closed universe start its evolution from , for , , for and , for and for flat universe start its evolution from , for , , for and , for but ends at
the ( , ) in the future for the open, flat and closed universes. One can also observe from this figure that the Tsallis HDE model would tends to the flat model in the future for the open, flat and closed universes. The () plane behaviour of Tsallis HDE models differs from [63].
From Fig. 6, in evolutionary plane, we observe that the Tsallis HDE model evolutionary trajectories started from matter dominated universe i.e. SCDM ( , ) in the past, and their evolutionary trajectories approaches the
point (, ) in the future i.e. the de Sitter expansion () for the open, flat and closed universes. Moreover, the difference between them is minor, but we can see that, from Fig. 6, the distance from the de Sitter expansion for is less in an open universe in comparison to closed and flat universes. Setare et al. [60], have a diagnosis the HDE in the nonflat universe with future event horizon as IR cutoff where the focus was different values of parameter and the spatial curvature contributions. The () plane behaviour of THDE models also differs from [60].
These graphs demonstrate that the evolutionary trajectories with distinct display altogether various highlights in the statefinder plane, which has been talked about in detail in [73, 74]. Presently we are keen on the analysis to the spatial curvature contributions in the derived models utilizing the statefinder parameters as a test. It has unmistakably appeared in Fig 5. also, Fig. 6, that the statefinder analysis has the intensity of testing the contributions of spatial curvature.
Curvature 
=0.0027 (open universe)  = 0.01 (Closed Universe)  = 0 ( Flat Universe)  

Parameter  = 1.5  = 1.7  = 1.9  = 1.5  = 1.7  = 1.9  = 1.5  = 1.7  = 1.9 
r  0.75403  0.886881  0.970638  0.727003  0.869757  0.965314  0.741921  0.879249  0.968279 
s  0.985806  0.0395844  0.00944539  0.115778  0.047642  0.0115643  0.106509  0.0432623  0.0104058 
q  0.333056  0.453901  0.537545  0.280977  0.406264  0.494803  0.307692  0.43038  0.516129 
0.777986  0.891026  0.969267  0.759398  0.880448  0.965994  0.769231  0.886076  0.967742  
0.288089  0.185484  0.0619011  0.284372  0.189938  0.0650366  0.286755  0.187835  0.063442  

5.1 Analysis of the pair
In this section, the dynamical feature of the Tsallis HDE, as an enhancement to the statefinder analysis, in plane has investigated. This diagnostic received recognition to some extent for examining DE models. In the plane, the scopes of quintessence DE and its behaviour have researched in [72]. Forwarding this point, by considering the dynamical property of other DE models including progressively more wide models was being utilized from the viewpoint [105, 106, 107], etc.. Recently the comparison among different DE models has been explored by the plane [70]. The plane investigation provides us with an elective technique without uncertainty for classification of models of dark energy using the parameters depicting the dynamical property of DE. The estimation of the statefinder method is that the statefinder parameters are worked from the scale factor and its differential coefficient, and they are regularly to be evacuated in a modelselfgoverning way from observational data in spite of the way that it seems hard to achieve this at present. While the upside of the examination is that it is a direct dynamical investigation for DE. In this way, the statefinder is the geometrical end and the dynamical assurance can be viewed as complementarity in some sense.
Now, we will examine the THDE in the plane. Fig. 7 demonstrates an illustrative precedent in which we plot the transformative directions of the THDE model in the plane for various Tsallis parameter and furthermore various spatial curvature contributions, as  0.0027, 0 and 0.01 comparing to the open, closed and flat universes, separately. The arrow in the plots represents the evolutionary direction. We plainly observe that the parameter assumes an important role in the derived model: the THDE behaves as quintessence type dark energy with , for all three values of parameter and different spatial curvature contributions. As appeared in these diagrams, the value of decreases monotonically while the value of first decreases to a minimum then increases to zero. The effect of curvature contribution may be identified explicitly in this diagram, although the difference is minor. Henceforth, we see that the dynamical conclusion may outfit with an important enhancement to the statefinder geometrical investigation.
6 Conclusion
We have explored the THDE in the nonflat universe within the framework of General Relativity filled with
matter and THDE considering apparent horizon as IR cutoff from the statefinder and pair viewpoint. We have acquired different parameters of cosmology to comprehend the decelerated to the accelerated evolution of the universe in our described model. Main results are concluded as
We inspect the DP of our model for different Tsallis parameter for distinct spatial curvature contributions and represents decelerated to accelerating phases of the universe depending on the parameter and also the type of spatial curvature, which is in good agreement with the current observations.
In the proposed THDE model, the EoS parameter deviates in quintessence scenario and reaches to , at the future for different Tsallis parameter in different spatial curvature contributions. The model shows affirmity to CDM model for all three values of in open, flat and closed universes.
As suggested by various cosmological observations that the universe is in accelerated expansion phase presently, the numerous cosmological models including the modified gravity or DE have been proposed to translate this grandiose accelerated expansion. This prompts the issue of how to segregate between these different candidates. The statefinder analysis gives a helpful mechanism to break the conceivable depravity of various cosmological models by establishing the parameters utilizing the higher differential coefficient of the scale factor. In this way, the strategy for plotting the evolutionary trajectories of DE models in the statefinder plane can be utilized as a diagnostic tool to separate between various models.
Also, despite the fact that we are missing with regards to a fundamental hypothesis for the DE, this hypothesis is attempted to have a few highlights of a quantum gravity hypothesis, which can be investigated theoretically by considering the holographic rule of quantum gravity hypothesis. So THDE model gives us an endeavour to investigate the nature of DE inside a structure of the fundamental theory.
pair and the statefinder pair plots demonstrate that the spatial curvature contributions in the model can be analyzed expressly in this technique.
The present values of the paramters and for different Tsallis parameter in different spatial curvature contributions are summarised in Table 2.
The scenario of THDE guides to fascinating cosmological phenomenology. The universe shows the regular thermal history, in particular, the progressive order of the matter and DE period, with the change from deceleration to speeding up occurring, previously it results in a completely DE domination in future.
Important results of our analysis is that the Tsallis HDE model is not quite the same as other DE models, for example, Holographic dark energy, Ricci dark energy from the statefinder perspective and furthermore not the same as these with and NADE from the pair perspective.
The composite null diagnostic and statefinder hierarchy are subjected to be examined in future to turn out to be all the more near the features of Tsallis HDE.
Acknowledgments
The authors are appreciative to IUCAA, Pune, India for offering help and office to do this research work. The authors are also appreciative to A. Pradhan for his fruitful suggestions which improved the paper in present form.
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