Research Article | Open Access

D. D. Pawar, V. R. Patil, S. N. Bayaskar, "Spherically Symmetric Fluid Cosmological Model with Anisotropic Stress Tensor in General Relativity", *International Scholarly Research Notices*, vol. 2012, Article ID 965164, 10 pages, 2012. https://doi.org/10.5402/2012/965164

# Spherically Symmetric Fluid Cosmological Model with Anisotropic Stress Tensor in General Relativity

**Academic Editor:**W.-H. Steeb

#### Abstract

This paper deals with the cosmological models for the static spherically symmetric spacetime for perfect fluid with anisotropic stress energy tensor in general relativity by introducing the generating functions and and also discussing their physical and geometric properties.

#### 1. Introduction

The study of anisotropic fluid sphere and gravitational collapse problem is important in relativistic astrophysics. Ruderman [1] investigated relativistic stellar model and shows that the stellar matter may be anisotropic at very high density ranges. Anisotropy in fluid pressure could be introduced by the existences of solid core by the presence of type 3A superfluid. Rago [2] presented the procedure to obtain the solution of the field equations by using two arbitrary functions in Einstein general relativity where two arbitrary functions are introduced: the anisotropic function that measures the degree of anisotropy and a generating function. These functions determine the relevant physical variables as well as metric coefficients. Kandalkar and Khadekar [3] have obtained analytical solutions for anisotropic matter distribution in the context of bimetric theory of gravitation. The dynamical equations governing the gravitational nonadiabatic collapse of a shear-free spherical distribution of anisotropic matter in the presence of charge have been studied by Tikekar and Patel [4]. According to Ruderman [1] and Canuto [5], the pressure in the various gravitational collapse of spherical distribution consisting of super dense matter distribution, may not be isotropic throughout for such stars; the core region may be anisotropic. Gair [6] obtained the spherical universes with anisotropic pressure. Thomas and Ratanpal [7] studied various aspects of gravitational collapse by using analytical and numerical methods by considering the gravitational collapse for spherical distributions, consisting of superdense matter distribution. In the last few years there has been increasing interest in the interior solutions of Einstein field equations corresponding to fluid distributions with anisotropic pressures Letelier [8], Maharaj and Maartens [9], Bondi [10], Coley and Tupper [11], and Singh et al. [12]. The matter distribution is adequately described by perfect fluid due to the large-scale distribution of galaxies in our universe. Hence a relativistic treatment of the problem requires the consideration of material distribution other than the perfect fluid.

In this paper, we have obtained cosmological models for static spherically symmetric spacetime with anisotropic stress energy tensor by introducing two generating functions and โโand also discussed their physical properties.

#### 2. Field Equations

Consider the static spherically symmetric space-time: where and being the function of alone.

The energy momentum tensor for perfect fluid with anisotropic stress energy with heat flux is given by where denote the matter density, fluid pressure, heat conduction vector orthogonal to , and components of unit time-like flow vector field of matter, respectively, And the anisotropic stress energy tensor is given by where symbolizes the magnitude of the anisotropic stress tensor and the radial vector is obtained as By choosing the commoving system, yields The energy momentum tensor (2.2) with (2.3) has the following nonvanishing components: The pressure along radial direction, is different from the pressure along the tangential direction, Using (2.7) and (2.8), the magnitude of anisotropic stress tensor is The Einstein field equations for space-time (2.1) with (2.6) yield where the prime over the letters indicates the derivative with respect to .

The consequence of conservation of energy momentum tensor leads to From (2.12), where = mass function.

Again, from (2.13) we obtain Using (2.14), (2.15), and then (2.10) yields Now, we define generating function and also introduce the anisotropic function , respectively, as From (2.17) and (2.18), we can obtain , and the metric potentials are as follows.

Using (2.17) and (2.18) in (2.16), Differentiating (2.14) yields Adding on both sides of (2.12) and using (2.20) and (2.17), we obtain Differentiating (2.17) yields On simplifying (2.21) and (2.22), we get Equation (2.23) is linear differential equation in . We obtain its solution as where is constant of integration and , โ are, Equation (2.14) yields Putting this value in (2.22) and using (2.17), we obtain which is the expression for effective density .

Equation (2.18) yields, From (2.14) and (2.17), we have From (2.10) and (2.29), where is constant of integration.

By using (2.28) and (2.29) the space-time (2.1) becomes The cosmological model (2.31) is physically meaningful with (2.9), (2.24), (2.25), and (2.27).

Here we consider the following three cases.

*Case 1. * We define the generating function from (2.17) and (2.18) as
Whare is a constant such that , and this choice should lead to a physically reasonable model since the function as that implies the Minkowskian space via (2.29), then the (2.25) yields,
Equation (2.24) and hence (2.7) yield
If the constant, then .

Hence from (2.25),
Also from (2.27) and (2.35) we obtain
Using (2.32) and (2.33), (2.29) and (2.30) give
where .

Using (2.38), the cosmological model for the space-time (2.1) is,

*Case 2. *We choose the generating function as
From (2.25),
where .

From (2.40) we obtain
From (2.7) we get
where .

From (2.25),
The metric potentials in (2.29) and (2.30) become
The space-time (2.1) can be written as

*Case 3. *When , then (2.18) gives
On (2.10) and (2.11), we have
With (2.13), (2.49), and (2.50), we obtain
On integrating, we get
where , is the constant of integration.

Subtracting (2.12) from (2.10), we get
Equations From (2.52) and (2.53) yield
On differentiating and simplifying (2.12), we get
where .

Using (2.54) and (2.55) we have
where and , is the constant of integration.

Thus the space-time (2.1) becomes
Equation (2.57) perfectly matches with Schwarzschild interior solution with

#### 3. Discussion

The cosmological model (2.31) is physically meaningful with radial pressure , tangential pressure , and energy density being given by (2.24), (2.28), and (2.27) respectively. The model has initial singularity at .

Here we discuss the following three cases.

In Case 1, we consider generating function and anisotropic function as defined in (2.32) and (2.33) such that and the radial pressure and energy density become constant.

In Case 2, as and the pressure , energy density , and stress tensor all are infinite, the model starts with big bang. As , , the model (2.48) represents a vacuum model.

While in Case 3, we consider this gives; which implies that the cosmological model (2.57) is isotropic with pressure density given by (2.58), and our result perfectly matches with Schwarzschild interior solution.

#### 4. Conclusion

We have investigated the spherically symmetric cosmological model for perfect fluid with anisotropic stress tensor in general relativity. Here we discuss the three different cases in which the last case for matches with the Schwarzschild interior solution.

#### Acknowledgement

The authors are grateful to the referee for his valuable comments and suggestions.

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#### Copyright

Copyright © 2012 D. D. Pawar et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.