Received 11 December 2015; accepted 26 March 2016; published 30 March 2016
Recent cosmological measurements obtained by SNe Ia   , WMAP  , SDSS  and X-ray   indicate that our universe is expanding and the expansion of the universe is accelerating. The notion known as dark energy (DE) with large negative pressure is proposed to explain this phenomenon which marks the beginning of a new era in cosmology. At present there are a lot of theoretical models of dark energy. Cosmological constant is the simplest model of dark energy corresponding to the model. Besides cosmological constant, the other dark energy models are quintessence  , phantom  , tachyon  , holographic dark energy   , K-essence  and Chaplygin gas models with various equation of state. Our universe consists of about 70% dark energy, 25% dark matter and 5% normal matter (Cold matter and Baryons) and negligible radiation according to the cosmological measurements and analysis. For the accelerated expansion of the universe filled with fluids, the pressure p and the energy density of the universe should violate the strong energy condition i.e., pressure must be negative to accelerate the expansion of the universe.
In Chaplygin gas (CG) the equation of state parameter for dark energy can be less than −1 as based on the observational data where the equation of state (EoS)  is,. The Chaplygin gas is connected to string theory which can be obtained by the Nambu-Goto action moving in a -dimensional space-time in the light-cone parametrization  . The transition period can be described when the universe is filled with Chaplygin gas from a decelerated cosmological expansion to the present exponentially accelerated
universe. A viable model  -  is introduced by generalizing the above equation to the form with, which is known as generalized Chaplygin gas (GCG), consisting of two free parameters B and respectively. At high density the generalized Chaplygin gas corresponds to a dust universe which
is not applicable to our universe. Therefore, modified Chaplygin gas (MCG) was introduced by Benaoum   with the equation of state,. This equation of state describes the evolution of the universe for small values of the cosmological scale factor corresponding to radiation era as well as for large values of the cosmological scale factor corresponding to model. The modified Chaplygin gas may be equivalently described in terms of a homogeneous minimally coupled scalar field in a Friedmann model.
Generalized Cosmic Chaplygin gas   was introduced in 2003 by P. F. Gonzalez-Diaz. This model can be made to be stable and free from unphysical behaviors even when the vacuum fluid satisfies the phantom energy condition, which is the striking factor of this model. The equation of state of Generalized Cosmic Chaplygin gas is
where with A being a constant that can take on both positive and negative values and; L being a positive definite constant, which can take on values larger than unity.
W. Chakraborty and U. Debnath et al.  has obtained the acceleration of the universe containing the modified Chaplygin gas and barotropic fluid. J. K. Singh et al.  within the framework of Lyra’s geometry studied the modified Chaplygin gas with statefinder parameters. In this paper we try to observe the state of the universe by using Generalized Cosmic Chaplygin gas and barotropic fluid and obtain the values of the statefinder parameters.
2. Field Equations and Their Solutions
The metric of a homogenous and isotropic universe in FRW model is
where is the scale factor and is the curvature scalar.
The Einstein field equations are (for)
The energy conservation equation is
For Generalized Cosmic Chaplygin gas, Equation (5) yields
where B is an arbitrary integration constant.
We consider two fluid cosmological model containing a component of Generalized Cosmic Chaplygin gas, with equation of state (5) and also a component of barotropic fluid with equation of state. satisfies
for accelerating universe normally. But satisfies according to observations i.e., corresponds to phantom model. The right hand side of Equations (3) and (4), i.e. and p should be
replaced by and for these two fluid components respectively. We assumed that the two fluids are conserved separately. For Generalized Cosmic Chaplygin gas the expression for the density is given by Equation (6). For another fluid, from Equation (5) the expression for density is given by
where d is an integration constant.
Now to derive the expression for the potential, the following Lagrangian is considered
The analogous energy density and pressure corresponding scalar field having a self interacting potential are given by
Now for flat universe () and assuming we have the expression for and as follows
For simplicity we have studied where the two fluids for early universe coincide at higher densities.
3. The Statefinder Parameters
It was of utmost necessity to devise a method that would both qualitatively and quantitatively discriminate between various dark energy models, as numerous dark energy models began appearing. Sahni et al. in 2003 pro-
posed a pair of parameters, called statefinder parameters in this context. In a independent manner these
parameters are able to discriminate between different dark energy models. The statefinder diagnostic pair has the following form
where and are the Hubble parameter and the deceleration parameter respectively. These
parameters allow us to characterize the properties of dark energy as these are dimensionless. Corresponding to different cosmological models, trajectories in the plane corresponds to the fixed point .
These statefinder parameters for one fluid model are given by
Equations (14) and (15) take the following form for the two fluid components,
The deceleration parameter q has the form
For Generalized Cosmic Chaplygin gas and barotropic equation of state,
Thus Equations (16) and (17) can be written as
Now for cosmic acceleration and since we get. The ratio between energy density of the barotropic fluid to that of Generalized Cosmic Chaplygin gas is denoted by y and the ratios of fluid pressure to energy density for barotropic fluid and Generalized Cosmic Chaplygin gas is denoted by respectively. We can assign different values to the barotropic index, since is constant. But at least one of the fluids must generate negative pressure for cosmic acceleration.
For different values of we get different cases which are as follows:
Case 1): For, we get which corresponds to a universe having cosmic acceleration but unable to violate the strong energy condition as it does not contain barotropic fluid;
Case 2): For and it also corresponds to cosmic acceleration and here Chaplygin gas violates the strong energy condition. The barotropic fluid represents the dust;
Case 3): For we get cosmic acceleration and here the Chaplygin gas does not violate the strong energy condition;
Case 4): For the Chaplygin gas represents the dark energy or the dark matter depending upon the values of x and the barotropic fluid represents the phantom model.
The pair of parameters (r, s) called statefinder parameters distinguish between different types of dark energy. The statefinders were introduced to characterize flat universe models with cold matter (dust) and dark energy. In this paper we have discussed the universe filled with two fluids, Generalized Cosmic Chaplygin gas and barotropic fluid to observe the phases of the universe when it undergoes acceleration using the statefinder parameters and obtain different situations depending upon the values of where both the fluids represent dark energy and sometimes dark matter. By considering the mixture of the two fluids, we observe the accelerating phase of the universe from the radiation era to for and the radiation era to quintessence model for. When, then which corresponds to cosmic acceleration, not violating strong energy condition; when, then which corresponds to cosmic acceleration, violating strong energy condition. When, then it corresponds to cosmic acceleration where Chaplygin gas does not violate strong energy condition and when, then Chaplygin gas represents dark energy or dark matter and barotropic fluid represents phantom model.
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