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Advances in Mathematical Physics

Volume 2014 (2014), Article ID 290459, 6 pages

http://dx.doi.org/10.1155/2014/290459

## The Deng Algorithm in Higher Dimensions

Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, Durban 4000, South Africa

Received 10 November 2013; Accepted 6 December 2013; Published 9 January 2014

Academic Editor: B. G. Konopelchenko

Copyright © 2014 Y. Nyonyi 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.

#### Abstract

We extend an algorithm of Deng in spherically symmetric spacetimes to higher dimensions. We show that it is possible to integrate the generalised condition of pressure isotropy and generate exact solutions to the Einstein field equations for a shear-free cosmological model with heat flow in higher dimensions. Three new metrics are identified which contain results of four dimensions as special cases. We show graphically that the matter variables are well behaved and the speed of sound is causal.

#### 1. Introduction

Spherically symmetric gravitating models with heat flow, in the absence of shear, are important in the study of various cosmological processes and the evolution of relativistic astrophysical bodies. For a variety of applications in the presence of inhomogeneity, see Krasinski [1]. Heat flow models are also important in analysing gravitational collapse and relativistic stellar processes. Astrophysical studies in which heat flow is important include the shear-free models of Wagh et al. [2], Maharaj and Govender [3], Misthry et al. [4], and Herrera et al. [5]. By studying shear-free models, we avail ourselves with a rather simpler avenue where we only need to provide solutions to the generalised condition of pressure isotropy containing two metric functions. A complete study of shear-free heat conducting fluids with charge was completed by Nyonyi et al. [6] using Lie’s group theoretic approach applied to differential equations. Shearing models where heat flow is significant have been recently studied by Thirukkanesh et al. [7] for radiating spherically symmetric spheres. It turns out that the resulting nonlinear equations with shear are much more difficult to analyse.

A generic method of obtaining new solutions to the Einstein field equations with heat flow was provided by Deng [8]. Using this general method, we can regain existing results and obtain new classes of solutions. Nyonyi et al. [6], Ivanov [9], and Msomi et al. [10] have obtained new solutions using the Lie group theoretic approach and other methods, by solving the underlying pressure isotropy condition. These investigations are applicable to four dimensions. Extensions to higher dimensions have also been considered by many authors because of physical requirements; for example, Bhui et al. [11] showed the absence of horizons in nonadiabatic gravitational collapse. Studies of this type motivated the Lie symmetry analysis of heat conducting fluids by Msomi et al. [12] in dimensions greater than four. In the present treatment, we extend the Deng [8] algorithm to higher dimensions and show that new results are possible.

#### 2. The Model

We consider the line element of a shear-free, spherically symmetric -dimensional manifold in the form where . The gravitational potential components and are functions of and with For a heat conducting fluid, the energy momentum tensor is given by where is the energy density, is the kinetic pressure, is the heat flux tensor, and is a timelike -velocity vector. For a comoving observer, we have and .

Utilizing (1)–(3), we obtain the Einstein field equationswhich are consistent with the derivation of Bhui et al. [11]. Equations (4b) and (4c), together with the transformation , give the pressure isotropy condition which is the master equation for the gravitating fluid in -dimensions.

Deng [8] provided a general recipe for generating a series of solutions of the isotropy condition (5) for . This technique may be extended to the master equation (5). Note that the isotropy condition is an ordinary differential equation in (since no time derivatives appear) which may be reduced to a simpler differential equation in if is known and vice versa. In this technique, the elementary forms of either or are chosen that are in turn substituted into the equation to be solved so as to obtain the form of the remaining term. Below we give a brief outline of the method.(1)Take a simple form of , say , and substitute it into the master equation to find the most general solution of , say . The pair and provides the first class of solutions to (5).(2)Take and substitute it into the master equation. This gives an equation in with already a solution. We are now in a position to obtain a second solution linearly independent of . The linear combination gives the general solution that satisfies the master equation. The pair and is the second class of solutions to (5).(3)Take and substitute it into the master equation. We obtain an equation in with already a solution. We are then in a position to obtain in the same way we obtained . The pair and is the third class of solutions to (5).(4)Repeat the above process to obtain an infinite sequence of solutions.

It is important to note that, in principle, this is a nonterminating process for obtaining solutions, and an infinite number of solutions can be listed. The difficulty arises in obtaining subsequent solutions in the process because the integration may become more complicated. However, the algorithm proves to be a powerful mechanism for generating new solutions.

#### 3. Results

We start with a simple case Equation (5) reduces to This equation can be solved directly to obtain where and are arbitrary functions of . The pair of equations (6) and (8) gives the first class of solutions Observe that the dimension is absent in metric (9). In this class of solutions the potentials are independent of the dimensionality; however, the spatial volume depends on and the matter variables are affected through the field equations. When , we regain the results of Bergmann [13].

On substituting (8) back into (5) we obtain The general solution to (10) is with and arbitrary functions of . The pair of equations (8) and (11) gives the second class of solutions Again, we observe that the dimension does not appear explicitly in (12). This means that the potentials in (12) are independent of the dimension. When , we regain the solutions obtained by Maiti [14] and later generalised by Modak [15] and Sanyal and Ray [16]. We make the general point that, for a linear form of , the parameter does not appear in (5). Thus all solutions with a linear form of do not contain the dimension , thereby leading to the metrics (9) and (12).

Now, substituting (11) into (5), we obtain We require two independent solutions and of (13). Note that in (8) is a solution to (13). We propose the second solution to (13) to be given by where the function has to be found explicitly. On substituting (14) into (13), we obtain On integrating (15), we obtain expressed as Consequently, the second solution will depend on the dimension . To evaluate integral (16), we need to consider two cases: and .

##### 3.1. Case I

When we have where is an arbitrary function of . Therefore becomes This implies that is proportional to and is therefore not a second linearly independent solution. The case is degenerate.

##### 3.2. Case II

When , we have where , , , , , and are arbitrary functions of . Therefore the second solution becomes And since the general solution to (5) is a linear combination of and , we obtain where we have introduced for convenience and . The third class of solutions is therefore given by (11) and (21) with metric This is a new class of solutions and it is evident that it certainly depends on the dimension . Therefore we can conclude that the dimensionality of the problem does indeed affect the dynamics of the gravitational field with heat flow. The next class of solutions can be obtained by substituting into (5) and then solving the resulting equation for . This may be continued to obtain further new solutions. The integration process gets more complicated for further iterations.

We now consider the special case of four dimensions. When and , the line element (22) becomes We can rewrite (23) in the equivalent form where the function is given by When we set in (24), we regain the result of Deng [8]. We interpret (22) as the higher dimensional generalisation of the Deng model with heat flow.

#### 4. Example

We illustrate the validity of our solutions by considering a simple example with physically viable conditions. For the line element (22), we make the simple choice: , , , and . This gives the simplified forms of the potentials Even with this simple example, a qualitative analysis of the matter variables and energy conditions for the interior matter distribution is arduous. We therefore generate graphical plots on a constant timelike hypersurface to illustrate the validity of our solutions using this example. Figures 1, 2, and 3 are the plots for the energy density , the pressure , and the heat flow for three different dimensions: (dashed line), (solid line), and (dotted line). It is clearly evident that the matter variables are positive and they decrease with the increase in dimension. This is due to the fact that an increase in dimension translates to an increase in the number of degrees of freedom leading to a decrease in the mass per unit volume of the gravitating fluid. In Figure 4, we have plotted the speed of sound. From Figure 4, we observe that causality is not violated for the dimensions , , and . In Figures 5, 6, and 7, we have plotted the quantities , , and , where for . We observe that , , and are positive; hence, the weak, dominant, and strong energy conditions are satisfied. Therefore the matter distribution for this example is physically reasonable.

#### 5. Discussion

We obtained new generalised classes of exact solutions to the Einstein field equations for a neutral relativistic fluid in the presence of heat flow in a higher dimensional manifold. We found new solutions to the coupled Einstein system by solving the higher dimensional pressure isotropy condition which is a second order nonlinear differential equation. We solved the master equation by making use of the Deng algorithm [8] and obtained three new metrics. The first metric (9) generalises the Bergmann [13] line element. The second metric (12) generalises the Maiti [14], Modak [15], and Sanyal and Ray [16] line elements. It is remarkable that the potentials in (9) and (12) are independent of the dimension. The third metric (22) depends on the dimension and generalises the Deng [8] line element. We conclude that the dimension of the spacetime affects the dynamics of the heat conducting gravitating fluid. We briefly studied the physical features by graphically plotting the matter variables. The energy conditions are found to be positive and causality is not violated.

#### Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

#### Acknowledgments

Y. Nyonyi, K. S. Govinder and S. D. Maharaj thank the National Research Foundation and the University of KwaZulu-Natal for their financial support. S. D. Maharaj further acknowledges that this research is supported by the South African Research Chair Initiative of the Department of Science and Technology.

#### References

- A. Krasinski,
*Inhomogeneous Cosmological Models*, Cambridge University Press, Cambridge, UK, 1997. - S. M. Wagh, M. Govender, K. S. Govinder, S. D. Maharaj, P. S. Muktibodh, and M. Moodley, “Shear-free spherically symmetric spacetimes with an equation of state $p=\alpha \rho $,”
*Classical and Quantum Gravity*, vol. 18, no. 11, pp. 2147–2162, 2001. View at Publisher · View at Google Scholar · View at Scopus - S. D. Maharaj and M. Govender, “Radiating collapse with vanishing weyl stresses,”
*International Journal of Modern Physics D*, vol. 14, no. 3-4, pp. 667–676, 2005. View at Publisher · View at Google Scholar · View at Zentralblatt MATH · View at MathSciNet - S. S. Misthry, S. D. Maharaj, and P. G. L. Leach, “Nonlinear shear-free radiative collapse,”
*Mathematical Methods in the Applied Sciences*, vol. 31, no. 3, pp. 363–374, 2008. View at Publisher · View at Google Scholar · View at Scopus - L. Herrera, A. di Prisco, and J. Ospino, “Some analytical models of radiating collapsing spheres,”
*Physical Review D*, vol. 74, no. 4, Article ID 044001, 7 pages, 2006. View at Publisher · View at Google Scholar · View at Scopus - Y. Nyonyi, S. D. Maharaj, and K. S. Govinder, “New charged shear-free relativistic models with heat flux,”
*The European Physical Journal C*, vol. 73, article 2637, 2013. View at Publisher · View at Google Scholar - S. S. Thirukkanesh, S. S. Rajah, and S. D. Maharaj, “Shearing radiative collapse with expansion and acceleration,”
*Journal of Mathematical Physics*, vol. 53, no. 3, Article ID 032506, 2012. View at Publisher · View at Google Scholar · View at Scopus - Y. Deng, “Solutions of the Einstein equation with heat flow,”
*General Relativity and Gravitation*, vol. 21, no. 5, pp. 503–507, 1989. View at Publisher · View at Google Scholar · View at MathSciNet - B. V. Ivanov, “Collapsing shear-free perfect fluid spheres with heat flow,”
*General Relativity and Gravitation*, vol. 44, no. 7, pp. 1835–1855, 2012. View at Publisher · View at Google Scholar · View at Zentralblatt MATH · View at MathSciNet - A. M. Msomi, K. S. Govinder, and S. D. Maharaj, “New shear-free relativistic models with heat flow,”
*General Relativity and Gravitation*, vol. 43, no. 6, pp. 1685–1696, 2011. View at Publisher · View at Google Scholar · View at Scopus - B. Bhui, S. Chaterjee, and A. Banerjee, “Non-adiabatic gravitational collapse in higher dimensional space-time and its junctions conditions,”
*Astrophysics and Space Science*, vol. 226, no. 1, pp. 7–18, 1995. View at Publisher · View at Google Scholar · View at Scopus - A. M. Msomi, K. S. Govinder, and S. D. Maharaj, “Applications of lie symmetries to higher dimensional gravitating fluids,”
*International Journal of Theoretical Physics*, vol. 51, no. 4, pp. 1290–1299, 2012. View at Publisher · View at Google Scholar · View at Scopus - O. Bergmann, “A cosmological solution of the Einstein equations with heat flow,”
*Physics Letters A*, vol. 82, no. 8, p. 383, 1981. View at Publisher · View at Google Scholar · View at MathSciNet - S. R. Maiti, “Fluid with heat flux in a conformally flat space-time,”
*Physical Review D*, vol. 25, no. 10, pp. 2518–2520, 1982. View at Publisher · View at Google Scholar · View at MathSciNet - B. Modak, “Cosmological solution with an energy flux,”
*Journal of Astrophysics and Astronomy*, vol. 5, no. 3, pp. 317–322, 1984. View at Publisher · View at Google Scholar - A. K. Sanyal and D. Ray, “Cosmological solutions of the Einstein equation with heat flow,”
*Journal of Mathematical Physics*, vol. 25, no. 6, pp. 1975–1976, 1984. View at Publisher · View at Google Scholar · View at MathSciNet