Kanti Jotania

Magnetized String Cosmological Model in Cylindrically Symmetric Inhomogeneous Universe with Time Dependent Cosmological-Term Λ

Cylindrically symmetric inhomogeneous magnetized string cosmological model is investigated with cosmological term L varying with time. To get the deterministic solution, it has been assumed that the expansion (q) in the model is proportional to the eigen value s1 1 of the shear tensor si j. The value of cosmological constant for the model is found to be small and positive which is supported by the results from recent supernovae Ia observations. The physical and geometric properties of the model are also discussed in presence and absence of magnetic field.

Some inhomogeneous magnetized viscous-fluid cosmological models with varying Λ

Some cylindrically symmetric inhomogeneous viscous-fluid cosmological models with electromagnetic field are obtained. To get a solution a supplementary condition between metric potentials is used. The viscosity coefficient of bulk viscous fluid is assumed to be a power function of mass density. Without assuming anyad hoc law, we obtain a cosmological constant as a decreasing function of time. The behaviour of the electromagnetic field tensor together with some physical aspects of the model are also discussed.

Finch-Skea star in (2+1) dimensions

The Bañados et al. (Phys Rev Lett 69:1849, 1992) solution corresponding to the exterior space-time of a black hole in

A relativistic two-parameter core-envelope model of compact stars

(2+1)

Structural and Magnetic Properties of BaMg2Fe10O19 Hexaferrite Particles

dimensions has been found to be very useful to understand various aspects relating to the gravitational field of a black hole. We present here a class of interior solutions corresponding to the BTZ exterior by making use of a model presented by Finch and Skea (Class Quantum Grav 6:467, 1989) which was earlier found to be relevant for the description realistic stars in

Some Exact Bianchi Type-V Perfect Fluid Cosmological Models with Heat Flow and Decaying Vacuum Energy Density Λ: Expressions for Some Observable Quantities

(3+1)