Plane symmetric string cosmological models in self-creation theory of gravitation

Rao, V. U. M.; Vinutha, T.

doi:10.1007/s10509-009-0156-x

Cited by 28 publications

(14 citation statements)

References 24 publications

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“…Pradhan et al (2009) discussed various aspects of LRS Bianchi type-I cosmological model in self-creation theory. Rao and Vinutha (2010) deduced some results on plane symmetric string cosmological models in self creation theory of gravitation. Barber (2010) again reviewed his theory of self-creation.…”

Section: Introductionmentioning

confidence: 99%

Bianchi type-I magnetized radiating cosmological model in self creation theory of gravitation

Jain¹,

Jain²

2015

Astrophys Space Sci

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Section: Introductionmentioning

confidence: 99%

Bianchi type-I magnetized radiating cosmological model in self creation theory of gravitation

Jain¹,

Jain²

2015

Astrophys Space Sci

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“…Yadav et al (2007aYadav et al ( , 2007b have obtained the integrability of cosmic string in Bianchi type III space-time in presence of bulk viscous fluid by applying a new technique. Reddy (2003, , , Rao et al (2008aRao et al ( , 2008bRao et al ( , 2009Rao et al ( , 2010, Pradhan (2007Pradhan ( , 2009, Pradhan and Mathur (2008), and Pradhan et al ( , 2010 have studied string cosmological models in different contexts. Recently, Tripathi et al (2009Tripathi et al ( , 2010 have obtained cosmic strings with bulk viscosity.…”

Section: Introductionmentioning

confidence: 99%

LRS Bianchi type-II massive string cosmological model in General Relativity

Pradhan

Ram

Singh³

2010

Astrophys Space Sci

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The present study deals with locally rotationally symmetric (LRS) Bianchi type II cosmological model representing massive string. The energy-momentum tensor for such string as formulated by Letelier (Phys. Rev. D 28:2414, 1983) is used to construct massive string cosmological model for which we assume that the expansion (θ ) in the model is proportional to the shear (σ ). This condition leads to A = B m , where A and B are the metric coefficients and m is proportionality constant. For suitable choice of constant m, it is observed that in early stage of the evolution of the universe string dominates over the particle whereas the universe is dominated by massive string at the late time. Our model is in accelerating phase which is consistent to the recent observations of type Is supernovae. Some physical and geometric behavior of the model is also discussed.

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“…Notable exceptions include a handful of studies in f (R) gravity [75,76,78], teleparallel theories [79,80], brane worlds [81,82], Kaluza-Klein models [83,84], Lovelock [85,86], Gauss-Bonnet [87][88][89], BornInfeld [90][91][92] and bimetric [93][94][95][96][97][98][99][100] gravity theories, and a few other, less mainstream, alternatives [101][102][103][104][105], while more comprehensive bodies of work exist for strings in scalar-tensor theories [106][107][108][109][110][111][112][113][114][115][116][117][118][119][120][121], including string theoryinspired dilation gravity [122,123], and gravitational th...…”

Section: Introductionmentioning

confidence: 99%

Cosmic strings in $$f\left( R,L_m\right) $$ f R , L m gravity

Harkó

Lake

2015

Eur. Phys. J. C

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We consider Kasner-type static, cylindrically symmetric interior string solutions in the f (R, L m ) theory of modified gravity. The physical properties of the string are described by an anisotropic energy-momentum tensor satisfying the condition T t t = T z z ; that is, the energy density of the string along the z-axis is equal to minus the string tension. As a first step in our study we obtain the gravitational field equations in the f (R, L m ) theory for a general static, cylindrically symmetric metric, and then for a Kasner-type metric, in which the metric tensor components have a power law dependence on the radial coordinate r . String solutions in two particular modified gravity models are investigated in detail. The first is the so-called "exponential" modified gravity, in which the gravitational action is proportional to the exponential of the sum of the Ricci scalar and matter Lagrangian, and the second is the "self-consistent model", obtained by explicitly determining the gravitational action from the field equations under the assumption of a power law dependent matter Lagrangian. In each case, the thermodynamic parameters of the string, as well as the precise form of the matter Lagrangian, are explicitly obtained.

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Plane symmetric string cosmological models in self-creation theory of gravitation

Abstract: Plane Symmetric string cosmological models are presented in Barber's second self creation theory of gravitation and obtained Einstein's plane symmetric string cosmological models as a special case. Some physical and geometrical properties of the models are also discussed.

Cited by 28 publications

References 24 publications

Bianchi type-I magnetized radiating cosmological model in self creation theory of gravitation

Bianchi type-I magnetized radiating cosmological model in self creation theory of gravitation

LRS Bianchi type-II massive string cosmological model in General Relativity

Cosmic strings in $$f\left( R,L_m\right) $$ f R , L m gravity

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