 Open Access
 Total Downloads : 306
 Authors : S. D. Deo, G. S. Punwatkar, U. M. Patil
 Paper ID : IJERTV3IS041077
 Volume & Issue : Volume 03, Issue 04 (April 2014)
 Published (First Online): 17042014
 ISSN (Online) : 22780181
 Publisher Name : IJERT
 License: This work is licensed under a Creative Commons Attribution 4.0 International License
Some Investigation LRS Bianchi Type I Model in General Relativity
S. D. Deo
Head, Department of Mathematics

S. Science & Arts College, Bhadrawati, Dist.Chandrapur
442902(M.S) India

S. Punwatkar
Department of Mathematics Datta Meghe Institute of Engineering, Technology & Research, Sawangi (Meghe), Wardha (M.S), India

M. Patil
Head, Department of Mathematics Shri Shivaji Science College, Amravati444603 (M.S) India
AbstractLocally Rotationally symmetric (LRS) Bianchi typeI cosmological model is studied in the context of general theory of relativity with the matter cosmic cloud string and electromagnetic field respectively. Further some physical and kinematical properties are discussed.
Keyword LRS Bianchi Model, cosmic cloud string, electromagnetic field, general relativity.
MSC2010 classification 83C05, 83C15. PACS 98.80.k, 95.30.k, 98.80.Cq, 04.20.q.

INTRODUCTION
Spacetimes admitting a three parameter group of automorphisms are important in discussing the cosmological models. The case where the group is simply transitive over the 3dimensional, constant time subspace is particularly useful for two reasons. First, Bianchi has shown that there are only nine distinct sets of structure constants for groups of this type. Therefore, we can use algebra to classify the homogeneous Space times. The second reason for the importance of Bianchi type Space – times is the simplicity of the field equations.
When we study the Bianchi type models, we observe that
It is well known that the exact solutions of general theory of relativity for homogeneous space times belong to either Bianchi types or KantowskiSachs. For simplification and description of the large scale behavior of the actual universe, locally rotationally symmetric (Henceforth referred as to LRS) BianchiI spacetime has been widely studied. In order to study problems like the formation of galaxies of the process of homogenization and isotropization of the universe, it is necessary to study problems relating to inhomogeneous and anisotropic space time.Mazumder [1] has obtained cosmological solutions for LRS BianchiI spacetime filled with a perfect fluid with arbitrary cosmic scale functions and studied kinematical properties of the particular form of the solution. Mohanti [2,3] also obtained some solutions for the same field equations by using solution generation technique with the matter perfect fluid. Banerjee [4] studied Bianchi type I cosmologies with cosmic strings. Numbers of researches [517] have studied Bianchi Type I cosmological models in general relativity.

Metric and Field Equation
The LRS Bianchi type I line element is given by
the models contain isotropic special cases and they permit arbitrarily small anisotropic levels at some instant of
ds2 dt2 A2dt2 B2 (dy2 dz2 )
(2.1)
cosmic times.
Bianchi type cosmological models are important in the sense that these models are homogeneous and anisotropic, from which the process of isotropization of the universe is studied through the passage of time. Moreover, from the theoretical point of view, anisotropic universe has a greater
Where, A and B are the scale factor (metric potential) and function of the cosmic time t only (nonstatic case).
The Einstein field equation in the general relativity is given by
i i
1
generality than isotropic models. The simplicity of the field equations made Bianchi space time useful in constructing models of spatially homogeneous and anisotropic
R j
i
2
Rg j 8 kT j
(2.2)
cosmologies.
Hence, these models are to be known as suitable models of
Where, R j
is known as Ricci Tensor
i
our universe. Therefore, study of Bianchi type models create much more interest.
Now, we discuss LRS Bianchi type – I cosmological space
– times in general relativity. The present day observations indicates that the universe at large scale is homogeneous and isotropic, and we have accelerating phase of universe
And R gij R is the Ricci Scalar
ij
i
T j is energy momentum tensor for the matter.
Einsteins field equation (2.2) for line element (2.1) lead to
A B
A
2 A
R11 A A 2 B
(2.3)
Where, A = t ,
A t2
etc.
From equation (2.11) and (2.12) we get
22 B B
R
A B
A
B 2

B
(2.4)
=0 (2.14)
Thus, cosmic cloud string does not exist.
33 B B
R
A B
A
B 2

B
(2.5)
Hence Vacuum solution are
A
B
B 2
B
2 B 0
B
(2.15)
R44 A 2 B
Case I: – For Massive cloud string
(2.6)
A B A B
0
A B AB
(2.16)
Here we consider the energy momentum tensor for a cloud massive string is given by
j j j
B 2
2 A B 0
(2.17)
Ti viv

xi x
(2.7)
B AB
Where, is the rest energy density for a cloud of string with particles attached along the extension.
Solving the equation (2.15) to (2.17) we obtain
Thus, p
(2.8)
A e(kt k1 )
e(kt k2 )
(2.18)
Where, p is particle energy and is the tension density of the string.
B k k3
(2.19)
vi is the four vector representing the velocity of cloud of particles and xi is the four vector representing the direction anisotropy, i.e. z direction.
Where, ki s are constants of integration.
The corresponding vacuum cosmological model can be written as
Where vi
and xi
satisfy condition
(ktk2 )
2 2(ktk ) e2 2
ds dt e 1 dx k
(dy2 dz2 )
(2.20)
2
k 3
vv j 1 , x x j 1 and v xi 0
(2.9)
i i i
The field equation (2.2) together with (2.7) for the line element (2.1) subsequently lead to the following system of equation
Case II: – For electromagnetic field
Here, the energy momentum tensor for electromagnetic field is defined as
B 2
B
E j F F jr 1 F F ab g j
F
(2.21)
B
2 0
B
(2.10)
i ir
4 ab i
i
i
Where, E j is electromagnetic energy tensor and
j is
A
B
A B
electromagnetic field tensor.
0
A B AB
(2.11)
In comoving coordinate system, the magnetic field is taken
A
B
A B
along Zaxis so that the nonvanishing components of
8 k A B AB
(2.12)
electromagnetic field tensor Fij is F12 .
The first set of Maxwells equation
B 2
B
2 A B 8 k AB
(2.13)
Fij,k Fjk ,i Fki, j 0
Lead to
(2.22)
F12 = constant [Here F14 0 F24 F34 ]
(2.23)
The nonvanishing component of shear tensor ij
by
defined
Now from equation (2.21) we obtain the components of the electromagnetic field
ij ui; j u j;i
(g
3
ij uiu j ) are obtained as
1 2 3 4 2
AA A2
E1 E2 E3 E4 2A2 B2
(2.24)
11 3
Uing comoving coordinate system, the field equations for the matric (2.1) can be written as
BB B2 22 33 3
B 2
B 2
0
B
2 4 k
B A2 B2
(2.25)
44
Thus shear scale is obtained as
A
B
A B 2
1 A 2
B 2
4 k
A B AB A2 B2
(2.26)
2
2 A2
2 2
B2
(3.4)
A
B
A B 2
4 k
A B AB A2 B2
(2.27)

CONCLUSION
We have investigated nonstatic LRS Bianchi type I
B 2
2 A B
2
2 2
4 k
(2.28)
Cosmological models with the matter cosmic cloud string and electromagnetic field respectively and further observed
B
AB A B
that in this model cosmic cloud string as well as electromagnetic field does not exist and vacuum solutions
From equation (2.26) and (2.27) we have
F12 0
(2.29)
have been obtained.

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Here we observed that, in anisotropic bianchi type I cosmological model electromagnetic field does not exist. Thus we have a new set of vacuum field equations which are same as the case I equation (2.15) to (2.17). We obtain the same vacuum cosmological model defined as in equation (2.20).
3. Physical and Kinematical Properties The spatial volume for the model (2.1) is given by

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