Articles
Kyungpook Mathematical Journal 2018; 58(4): 761-779
Published online December 31, 2018
Copyright © Kyungpook Mathematical Journal.
On Weakly Z Symmetric Spacetimes
Uday Chand De
Department of Pure Mathematics, University of Calcutta 35, Ballygunge Circular Road, Kolkata 700019, West Bengal, India
e-mail : uc_de@yahoo.com
Received: February 2, 2018; Accepted: June 4, 2018
Abstract
The object of the present paper is to study weakly
Keywords: weakly Z symmetric manifolds, weakly Z symmetric spacetimes, dust fluid and viscous fluid spacetimes, Robertson-Walker spacetime, Weyl conformal curvature tensor.
1. Introduction
The present paper is concerned with certain investigations in general relativity by the coordinate free method of differential geometry. In this method of study the spacetime of general relativity is regarded as a connected four-dimensional pseudo-Riemannian manifold (
The Einstein’s equation [21] imply that the energy momentum tensor is of vanishing divergence. This requirement is satisfied if the energy momentum tensor is covariant constant. Chaki and Roy [7] proved that a general relativistic space-time with covariant constant energy momentum tensor is Ricci symmetric, that is, ∇
In 1993 Tam
where ∇ denotes the Levi-Civita connection and
According to Yano [33] a vector field
where
In a pseudo-Riemannian manifold (
where
where the scalar curvature
A pseudo-Riemannian manifold is said to be
where
where
Recently, Mantica and Suh studied pseudo Z symmetric Riemannian manifolds [15] and recurrent Z forms on Riemannian manifolds [16], that is, Riemannian manifolds on which the form Λ(
On the otherhand, Lorentzian manifolds with Ricci tensor
where
Geometers identify the special form (
Shepley and Taub [28] studied perfect fluid spacetimes with equation of state
are Robertson-Walker spacetimes.
Motivated by the above works, in the present paper we study (
The paper is organized as follows:
After introduction in Section 2, we prove that a (
2. Weakly Z Symmetric Spacetimes
In this Section we prove that a (
Substracting (
which implies
If possible, let
Taking a frame field and contracting (
which implies
Putting
since
In virtue of (
which implies
that is,
where
Thus we can state the following:
Theorem 2.1
We now consider a (
where
Using the
Let us suppose that the generator
where
Now
since
Now from (
Since
Thus we can state the following:
Theorem 2.2
3. Conformally Flat (WZS )4 Spacetimes
This section is devoted to study conformally flat (
where
Using (
Let
for all
for every
for all
for all
Theorem 3.1
4. (WZS )4 Spacetime Satisfying the Condition divC = 0
Suppose (
where {
In this section we assume that the (
Using (
Taking a frame field and contracting over
where
Putting
Using (
Putting
Using (
If possible, let
and
Again using (
Using (
Putting
since
Hence it follows that
for all
Now using
Since
Therefore we can state the following:
Theorem 4.1
Using (
since
Then using (
On the other hand, (
from which we get
since (∇
Putting
Then using (
which implies that
where
Using (
is closed. In fact,
Using (
Putting
From (
Let
and
Since (∇
Similarly, we get
Hence
Now [
Hence [
Theorem 4.2
From (
where
Therefore the vector field
Thus we obtain the following:
Theorem 4.3
Remark 4.4
In Theorem 3.2 of [16] the authors prove the above Theorem under a restriction on
Since
and consequently
being
Definition 4.5
An
where
The generalized Robertson Walker spacetime is thus the warped product −1 ×
Theorem 4.6.([9])
In view of these results if a (
Theorem 4.7
Finally, we consider (
where
where
Comparing (
Again from Theorem it follows that
Theorem 4.8
According to Petrov classification a spacetime can be devided into six types denoted by I, II, III, D, N and O [22]. Again Barnes [2] has proved that if a perfect fluid spacetime is shear free, vorticity free and the velocity vector field is hypersurface orthogonal and the energy density is constant over a hypersurface orthogonal to the velocity vector field, then the possible local cosmological structure of the spacetime are of Petrov type I, D or O. Thus from Theorem we can state the following:
Theorem 4.9
5. Dust Fluid and Viscous Fluid (WZS )4 Spacetimes
In a dust or pressureless fluid spacetime, the energy momentum tensor
where
where
where
Using (
Taking a frame field after contraction over
which implies
Again, if we put
which implies that
Combining
Therefore
using (
Theorem 5.1
Let us consider the energy momentum tensor
where
Using (
Putting
where
Again contracting (
where
Hence we can state the following:
Theorem 5.2
We now discuss whether a viscous fluid (
where
Using (
Putting
which implies
where
Thus we are in a position to state the following:
Theorem 5.3
6. Example of a (WZS )4 Spacetime
In this section we prove the existence of a (
We consider a Lorentzian manifold (
where
The only non-vanishing components of the Christoffel symbols, the curvature tensor, the Ricci tensor, the
We shall now show that this
We choose the associated 1-form as follows:
and
at any point x ∈ ℝ4.
Now
Clearly,
7. Conclusion
In general relativity the matter content of the spacetime is described by the energy momentum tensor
The physical motivation for studying various types of spacetime models in cosmology is to obtain the information of different phases in the evolution of the universe, which may be classified into three phases, namely, the initial phase, the intermediate phase and the final phase. The initial phase is just after the Big Bang when the effects of both viscosity and heat flux were quite pronounced. The intermediate phase is that when the effect of viscosity was no longer significant but the heat flux was till not negligible. The final phase, which extends to the present state of the universe when both the effects of viscosity and heat flux have become negligible and the matter content of the universe may be assumed to be perfect fluid. The study of (
Quasi Einstein manifolds arose during the study of exact solutions of the Einstein field equations. It is proved that a (
References
- Alías, L, Romero, A, and Sánchez, M (1995). Compact spacelike hypersurfaces of constant mean curvature in generalized Robertson-Walker spacetimes. Geometry and Topology of Submanifolds VII. River Edge, NJ: World Sci. Publ, pp. 67-70
- Barnes, A (1973). On shear free normal flows of a perfect fluid. Gen Relativity Gravitation. 4, 105-129.
- Beem, JK, Ehrlich, PE, and Easley, KL (1996). Global Lorentzian Geometry. Monographs and Textbooks in Pure and Applied Mathematics. New York: Marcel Dekker, Inc
- Brickell, F, and Clark, RS (1970). Differentiable manifolds. London: Van Nostrand Reinhold Company
- Chaki, MC (1988). On pseudo Ricci symmetric manifolds. Bulgar J Phys. 15, 526-531.
- Chaki, MC, and Maity, RK (2000). On quasi Einstein manifolds. Publ Math Debrecen. 57, 297-306.
- Chaki, MC, and Roy, S (1996). Spacetimes with covariant-constant energy-momentum tensor. Int J Theor Phys. 35, 1027-1032.
- Chaki, MC, and Saha, SK (1994). On pseudo-projective Ricci symmetric manifolds. Bulgar J Phys. 21, 1-7.
- Chen, B-Y (2014). A simple characterization of generalized Robertson-Walker spacetimes. Gen Relativity Gravitation. 46.
- De, A, Özgür, C, and De, UC (2012). On conformally flat almost pseudo-Ricci symmetric spacetimes. Internat J Theoret Phys. 51, 2878-2887.
- Eisenhart, LP (1949). Riemannian Geometry: Princeton University Press
- Hall, GS (2004). Symmetries and Curvature Structure in general Relativity. World Scientific Lecture Notes in Physics. Singapore: World Scientific
- Karchar, H (1982). Infinitesimal characterization of Friedmann Universe. Arch Math (Basel). 38, 58-64.
- Mantica, CA, and Molinari, LG (2012). Weakly Z Symmetric manifolds. Acta Math Hungar. 135, 80-96.
- Mantica, CA, and Suh, YJ (). Pseudo Z symmetric Riemannian manifolds with harmonic curvature tensors. Int J Geom Methods Mod Phys. 9, 1250004-2012.
- Mantica, CA, and Suh, YJ (). Recurrent Z forms on Riemannian and Kaehler manifolds. Int J Geom Methods Mod Phys. 9, -2012.
- Mantica, CA, and Suh, YJ (2014). Pseudo-Z symmetric space-times. J Math Phys. 55.
- Mantica, CA, and Suh, YJ (2016). Pseudo-Z symmetric space-times with divergence-free Weyl tensor and pp-waves. Int J Geom Methods Mod Phys. 13.
- Mikeš, J, and Rachunek, L . Torse-forming vector fields in T-symmetric Riemannian spaces., Steps in Differential Geometry, Proc. of the Colloq. on Diff. Geometry, 25–30 July, (2000), Debrecen, pp.219-229.
- Novello, M, and Reboucas, MJ (1978). The stability of a rotating universe. Astrophys J. 225, 719-724.
- O’Neill, B (1983). Semi-Riemannian Geometry with application to the Relativity. New York-London: Academic Press
- Petrov, AZ (1949). Einstein spaces. Oxford: Pergamon press
- Roychaudhury, AK, Banerji, S, and Banerjee, A (1992). General relativity, astrophysics and cosmology: Springer-Verlag
- Sánchez, M (1998). On the geometry of generalized Robertson-Walker spacetimes: geodesics. Gen Relativity Gravitation. 30, 915-932.
- Sánchez, M (1999). On the geometry of generalized Robertson-Walker spacetimes: curvature and Killing fields. J Geom Phys. 31, 1-15.
- Schouten, JA (1954). Ricci-Calculus. Berlin: Springer
- Sharma, R (1993). Proper conformal symmetries of space-times with divergence-free Weyl conformal tensor. J Math Phys. 34, 3582-3587.
- Shepley, LC, and Taub, AH (1967). Space-times containing perfect fluids and having a vanishing conformal divergence. Commun Math Phys. 5, 237-256.
- Srivastava, SK (2008). General Relativity and Cosmology. New Delhi: Prentice-Hall of India Private Limited
- Sthepani, H, Kramer, D, MacCallum, M, Hoenselaers, C, and Hertl, E (2003). Exact solutions of Einstein’s Field Equations: Cambridge Monographs on Mathematical Physics, Cambridge University Press
- Tamássy, L, and Binh, TQ (1993). On weak symmetries of Einstein and Sasakian manifolds. Tensor (NS). 53, 140-148.
- Yano, K (1940). Concircular geometry I, Concircular transformations. Proc Imp Acad Tokyo. 16, 195-200.
- Yano, K (1944). On the torse-forming directions in Riemannian spaces. Proc Imp Acad Tokyo. 20, 340-345.
- Zengin, FO (2012). M-Projectively flat spacetimes. Math Rep. 14, 363-370.