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Field equations in the presence of perfect fluid distribution are obtained in a scalar tensor theory of gravitation proposed by Brans and Dicke[1] with the aid of Bianchi type-II, VIII & IX metrics. Exact prefect fluid Bianchi type- IX cosmological model is presented since other models doesn’t exist in Brans-Dicke scalar tensor theory of gravitation. Some physical properties of the model are also discussed.

Brans and Dicke [

Brans-Dicke field equations for combined scalar and tensor field are

and

where is an Einstein tensor,

is the stress energy tensor of the matter, is the dimensionless coupling constant and comma and semicolon denote partial and covariant differentiation respecttively.

The equation of motion

is a consequence of the field Equations (1.1) and (1.2).

Several aspects of Brans-Dicke cosmology have been extensively investigated by many authors. The work of Singh and Rai [

Nariai [

Chakraborty [

In this paper we discuss Bianchi type-II, VIII & IX perfect fluid cosmological models in a scalar-tensor theory proposed by Brans and Dicke [

We consider a spatially homogeneous Bianchi type-II, VIII and IX metrics of the form

(2.1)

where are the Eulerian angles, and are functions of t only. It represents Bianchi type-II if and

Bianchi type-VIII if and

Bianchi type-IX if and

The energy momentum tensor for perfect fluid distribution is given by

where r is the density and is the pressure.

Also

In the co moving coordinate system, we have from Equations (2.2) and (2.3)

, and for (2.4)

The quantities and are functions of “t” only.

The field Equations (1.1), (1.2) & (1.3) for the metric (2.1) with the help of Equations (2.2), (2.3) and (2.4) can be written as

and

where “” denotes differentiation with respect to “t”.

When = 0, –1 & +1, the field Equations (3.1)-(3.6) correspond to the Bianchi type-II, VIII & IX universes respectively.

Using the transformation, , , where and are functions of “T” only.

The field Equations (3.1) to (3.6) reduce to

(3.8)

(3.9)

where “ ′ ” denotes differentiation with respect to “T”.

Since we are considering the Bianchi type-II, VIII and IX metrics, we have, & for Bianchi type-II, VIII and IX metrics respectively. Therefore, from the Equation (3.10), we will consider the following possible cases with.

1) and

2) and

3) and

CASE (1): and:

Here, we get

Without loss of generality by taking the constant of integration, we get

By using (3.13), the field Equations (3.7) to (3.12) will reduce to

(3.15)

where “ ′ ” denotes differentiation with respect to “T”.

From (3.14) and (3.15), we have

From (3.19), we observe that, we can’t find Bianchi type-II () and VIII () perfect fluid cosmological models in Brans-Dicke theory of gravitation. But we can get Bianchi type-IX perfect fluid cosmological model in Brans-Dicke theory of gravitation.

For, the field Equations (3.14)-(3.18) reduce to

From (3.20), (3.21) & (3.23), we get

Then from (3.24), we get

with the relation, where are arbitrary constants.

Using (3.25) & (3.26) in (3.20) & (3.21), we get

The corresponding metric can be written in the form

(3.29)

Thus (3.29) together with (3.27) and (3.28) constitutes an exact Bianchi type-IX perfect fluid cosmological model in Brans-Dicke scalar-tensor theory of gravitation.

PHYSICAL AND GEOMETRICAL PROPERTIES:

The volume element of the Bianchi type-IX perfect fluid cosmological model is given by

We can observe that the spatial volume decreases as time “” increases, i.e., the model is contracting. Also the model has initial singularity at,

The scalar expansion and shear are given by

for Bianchi type-IX perfect fluid cosmological model in Brans-Dicke theory of gravitation. The scalar expansion as and as. So, the rate of expansion is rapid as time decreases and it becomes slow as time increases. The shear scalar as and as. Thus the shape of universe changes uniformly. The deceleration parameter q is obtained as. The negative value of q indicates that the model is inflationary. Since

which confirms that the universe remains anisotropic throughout the evolution.

CASE (2): and:

In this case, where is a constant of integration, without loss of generality we can take.

Hence the field Equations (3.7) to (3.12) reduce to general relativity field equations with.

(3.31)

From (3.33), we get

Since, we will get only radiating universe in this case.

The field Equations (3.30) to (3.34) reduce to

(3.37)

From (3.36) to (3.38), we have

Then from (3.40), we get

where, and are arbitrary constants satisfying

,.

FOR BIANCHI TYPEII METRIC:

From (3.36)-(3.38), we get

The corresponding metric can be written in the form

Thus (3.45) together with (3.43) & (3.44) constitutes Bianchi type-II Perfect fluid radiating cosmological models in general theory of relativity.

FOR BIANCHI TYPE-VIII METRIC:

From (3.36)-(3.38), we get

The corresponding metric can be written in the form

Thus (3.48) together with (3.46) & (3.47) constitutes Bianchi type-VIII Perfect fluid radiating cosmological models in general theory of relativity.

FOR BIANCHI TYPE-IX METRIC:

From (3.36)-(3.38), we get

The corresponding metric can be written in the form

Thus (3.51) together with (3.49) & (3.50) constitutes Bianchi type-IX Perfect fluid radiating cosmological models in general theory of relativity.

PHYSICAL AND GEOMETRICAL PROPERTIES:

The volume element of the above three models [(3.45), (3.48) & (3.51)] are given by

where, sinhθ and sinθ respectively.

In the above expressions, the volume decreases as time increases if i.e., the models are contracting, the volume increases as time increases if i.e., the models are expanding and the volume is independent of time T if. Also the models have initial singularity at,.

The expansion and shear are equal for all Bianchi type-II, VIII & IX perfect fluid radiating cosmological models in general relativity. Which are given by

The deceleration parameter

It can be seen that for large “” the quantities and will become zero if. Also the quantities and tends to +∞ as if and tends to –∞ if.Thus the rate of expansion is rapid as time decreases, it becomes slow as time increases and the shape of universe changes uniformly. In the case of, we can see that the Spatial Volume “V” is independent of time “T” and, will become zero.

Also, since, the models are not isotropic for large T. The negative value of the deceleration parameter q shows that the models inflate except for m = 1.

CASE (3): and

Here, we get

Without loss of generality by taking the constant of integration, we get

Sincewhere is a constant of integration, without loss of generality we can take.

Hence the field equations (3.7) to (3.12) reduce to general relativity field equations with.

where “ ′ ” denotes differentiation with respect to “T”.

From (3.53) and (3.54), we have

From (3.58), we observe that, we can’t find Bianchi type II () and VIII () perfect fluid cosmological models of general relativity. But we can get only Bianchi type IX perfect fluid cosmological model of general relativity.

For, the field equations (3.53)-(3.57) reduce to

From (3.61), we get

Since from, we will get only radiating universe in this case.

Now from (3.59), (3.60) and (3.61), we have

From (3.64), we get

Using (3.65) in (3.59) & (3.60), we get

The corresponding metric can be written in the form

Thus (3.67) together with (3.66) constitutes Bianchi type-IX radiating perfect fluid cosmological model in general theory of relativity.

PHYSICAL AND GEOMETRICAL PROPERTIES:

The volume element of the model (3.67) is given by

Now the expression for expansion and shear are given by

for Bianchi type-IX perfect fluid radiating cosmological model in Brans-Dicke theory of gravitation. The spatial volume tends to zero as T→∞. Thus the model is contracting with the increase of time and also the model has no real singularity. The deceleration parameter q is obtained as. The negative value of q indicates that the model is inflationary. Also, since

which confirms that the universe remains anisotropic throughout the evolution.

Bianchi type space-times play a vital role in understanding and description of the early stages of evolution of the universe. In particular, the study of Bianchi type-II, VIII & IX universes are important because familiar solutions like FRW universe with positive curvature, the desitter universe, the Taub-Nut solutions etc correspond of Bianchi type-II, VIII & IX space-times. In view of the importance of Bianchi type-II, VIII & IX spacetimes and also since exact solutions offer an alternative and complementary approach to study various cosmological models, in this paper we have presented Bianchi type-II, VIII & IX perfect fluid cosmological models in BransDicke theory of gravitation.

In case of and, we can observe that the only Bianchi type-IX perfect fluid cosmological model exists in Brans-Dicke theory of gravitation. The model is anisotropic, inflationary and has initial singularity at,. Also established the non-existence of Bianchi type-II & VIII perfect fluid cosmological models in this theory. Since “a” is an arbitrary constant and “ω” is a coupling constant, it is always possible to assign specific values to “a” and “ω” to keep the pressure “p” (3.27) and density “ρ” (3.28) be always positive.

In case of and, we can observe that Bianchi type-II, VIII & IX perfect fluid radiating cosmological models of general relativity exist in this theory. The models have initial singularity at, and remain anisotropic throughout the evolution.

In case of and, we have obtained only Bianchi type-IX anisotropic radiating perfect fluid cosmological model of general relativity with. In this case also we have observed that Bianchi type-II & VIII cosmological models doesn’t exist in this theory.