Plane symmetric bulk viscous domain wall in Lyra geometry

Pradhan, Anirudh; Kumar, K. Sravan; Yadav, Anil Kumar

doi:10.1590/s0103-97332007000700003

Cited by 23 publications

(12 citation statements)

References 37 publications

(65 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Recently, Saha and Visinescu [62] and Saha et al [63] have studied B-I models with cosmic string in presence of magnetic flux. Recently, Pradhan et al [64][65][66][67][68][69][70], Casama et al [71], Bali and Chandnani [72,73], Kumar and Singh [74], Ram, Zeyauddin and Singh [75], Singh [76] and Rao, Vinutha and Santhi [77] have studied cosmological models based on Lyra's geometry in various contexts. Motivated by the above discussions, in this paper, the field equations in normal gauge for Lyra's manifold where gauge function β is taken as time dependent, have been solved for massive string in presence of perfect fluid distribution of matter by applying a variation law for generalized Hubble's parameter in B-I space-time.…”

mentioning

confidence: 99%

Anisotropic Bianchi Type-I String Cosmological Models in Normal Gauge for Lyra’s Manifold with Constant Deceleration Parameter

Pradhan

Singh

2010

Int J Theor Phys

Self Cite

View full text Add to dashboard Cite

The present study deals with a spatially homogeneous and anisotropic Bianchi type-I (B-I) cosmological models representing massive strings in normal gauge for Lyra's manifold by applying the variation law for generalized Hubble's parameter that yields a constant value of deceleration parameter. The variation law for Hubble's parameter generates two types of solutions for the average scale factor, one is of power-law type and other is of the exponential-law type. Using these two forms, Einstein's modified field equations are solved separately that correspond to expanding singular and non-singular models of the universe respectively. The energy-momentum tensor for such string as formulated by Letelier, P.S.: Phys. Rev. D 28, 2414 is used to construct massive string cosmological models for which we assume that the expansion (θ ) in the model is proportional to the component σ 1 1 of the shear tensor σ j i . This condition leads to A = (BC) m , where A, B and C are the metric coefficients and m is proportionality constant. Our models are in accelerating phase which is consistent to the recent observations. It has been found that the displacement vector β behaves like cosmological term in the normal gauge treatment and the solutions are consistent with recent observations of SNe Ia. It has been found that massive strings dominate in the both decelerating and accelerating universes. The strings dominate in the early universe and eventually disappear from the universe for sufficiently large times. This is in consistent with the current observations. Some physical and geometric behaviour of these models are also discussed.

show abstract

mentioning

confidence: 99%

Anisotropic Bianchi Type-I String Cosmological Models in Normal Gauge for Lyra’s Manifold with Constant Deceleration Parameter

Pradhan

Singh

2010

Int J Theor Phys

Self Cite

View full text Add to dashboard Cite

show abstract

“…Recently, Pradhan et al [26][27][28][29][30][31][32], Bali et al [33,34], Singh [35], and Rao et al [36] have studied the cosmological model based on Lyra's geometry with various matter distributions. Patil, Pawar and Deshmukh [37,38], have been obtained the plane symmetric cosmological models of thick domain wall coupled with viscous field.…”

Section: Introductionmentioning

confidence: 99%

Thick Domain Walls Coupled with Viscous Fluid and Electromagnetic Field in Lyra Geometry

2012

View full text Add to dashboard Cite

show abstract

“…As a natural consequences, we should include magnetic fields in the energy-momentum tensor of the early universe. The string cosmological models with a magnetic field are also discussed by Banerjee et al [11], Chakraborty [12], Tikekar and Patel [13,14], Patel and Maharaj [16], Singh and Singh [21], Bail et al [67,68], Pradhan et al [69][70][71][72][73]. Motivated the situations discussed above, in this paper, we shall focus upon the problem of establishing a formalism for studying the massive string in Bianchi III spacetime.…”

mentioning

confidence: 99%

Magnetized Bianchi Type III Massive String Cosmological Models in General Relativity

Amirhashchi

Zainuddin

2010

Int J Theor Phys

View full text Add to dashboard Cite

The present study deals with Bianchi type III string cosmological models with magnetic field. The magnetic field is assumed to be along z direction. Therefore F 12 is only the non-vanishing component of electromagnetic field tensor F ij . The expansion (θ ) in the model is assumed to be proportional to the shear (σ ). To get determinate solution in term of cosmic time, we have solved the fields equations in two cases (i) Reddy and (ii) Nambu string. The physical and geometrical behaviour of these models is discussed.

show abstract

Plane symmetric bulk viscous domain wall in Lyra geometry

Cited by 23 publications

References 37 publications

Anisotropic Bianchi Type-I String Cosmological Models in Normal Gauge for Lyra’s Manifold with Constant Deceleration Parameter

Anisotropic Bianchi Type-I String Cosmological Models in Normal Gauge for Lyra’s Manifold with Constant Deceleration Parameter

Thick Domain Walls Coupled with Viscous Fluid and Electromagnetic Field in Lyra Geometry

Magnetized Bianchi Type III Massive String Cosmological Models in General Relativity

Contact Info

Product

Resources

About