Ramesh Tikekar
Articles written in Pramana – Journal of Physics
Volume 39 Issue 1 July 1992 pp 17-25 Research Articles
Non-adiabatic gravitational collapse of charged radiating fluid spheres
Dynamical equations governing the non-adiabatic collapse of a shear-free spherical distribution of unisotropic matter in the presence of charge are obtained. A brief outline of constructing a model describing collapse of a charged radiating fluid sphere in the set up developed is given.
Volume 42 Issue 6 June 1994 pp 483-489
Some exact solutions in Bianchi VI_{0} string cosmology
Following the techniques used by Letelier and Stachel some new physically relevant explicit Bianchi VI_{0} solutions of string cosmology with magnetic field are reported. They include two models describing distributions of Takabayashi strings and geometric strings respectively.
Volume 49 Issue 2 August 1997 pp 213-224 Research Articles
Inhomogeneous cosmological models with heat flux
L K Patel Ramesh Tikekar Naresh Dadhich
We present a general class of inhomogeneous cosmological models filled with non-thermalized perfect fluid by assuming that the background spacetime admits two space-like commuting Killing vectors and has separable metric coefficients. The singularity structure of these models depends on the choice of the parameters and the metric functions. A number of previously known perfect fluid models follow as particular cases of this general class. Physical and geometrical features of these models are studied and the general expression for temperature distribution is given.
Volume 50 Issue 2 February 1998 pp 95-103
Relativistic fluid sphere on pseudo-spheroidal space-time
A new exact closed form solution of Einstein's field equations is reported describing the space-time in the interior of a fluid sphere in equilibrium. The physical 3-space,
Volume 52 Issue 3 March 1999 pp 237-244
Anisotropic fluid distributions on pseudo-spheroidal spacetimes
An exact solution of Einstein’s field equations for anisotropic fluid distribution on the background of a pseudo-spheroidal spacetime has been reported. The models based on this solution are found to accommodate density variation of high degree from the centre to the boundary of the distribution and admit a subclass for which both the radial and tangential pressures vanish at the boundary of the configuration.
Volume 55 Issue 3 September 2000 pp 361-368 Research Articles
Rotating cylindrically symmetric Kaluza-Klein fluid model
Kaluza-Klein field equations for stationary cylindrically symmetric fluid models in standard Einstein theory are formulated and a set of physically viable solutions is reported. This set is believed to be the first such Kaluza-Klein solutions and it includes the Kaluza-Klein counterpart of Davidson’s solution describing spacetime of a perfect fluid in rigid rotation about a regular axis.
Volume 55 Issue 4 October 2000 pp 623-628
On spherically symmetric singularity-free models in relativistic cosmology
The introduction of time dependence through a scale factor in a non-conformally flat static cosmological model whose spacetime can be embedded in a five demensional flat spacetime is shown to give rise to two spherical models of universe filled with perfect fluid acompannied with radial heat flux without any Big Bang type singularity. The first model describes an ever existing universe which witnesses a transition from state of contraction to that of ever expansion. The second model represents a universe oscillating between two regular states.
Volume 64 Issue 1 January 2005 pp 5-15
A relativistic core-envelope model on pseudospheroidal space-time
A core-envelope model for superdense matter distribution with the feature- core consisting of anisotropic fluid distribution and envelope with isotropic fluid distribution is reported on the background of pseudospheroidal space-time. The physical plausibility of the model is examined analytically and numerically.
Volume 68 Issue 3 March 2007 pp 397-406 Research Articles
On relativistic models of strange stars
The superdense stars with mass-to-size ratio exceeding 0.3 are expected to be made of strange matter. Assuming that the 3-space of the interior space-time of a strange star is that of a three-paraboloid immersed in a four-dimensional Euclidean space, we obtain a two-parameter family of their physically viable relativistic models. This ansatz determines density distribution of the interior self-gravitating matter up to one unknown parameter. The Einstein's field equations determine the fluid pressure and the remaining geometrical variables. The information about mass-to-size ratio together with the conventional boundary conditions lead to the determination of total mass, radius and other parameters of the stellar configuration.
Volume 79 Issue 2 August 2012 pp 211-222
Relativistic models of a class of compact objects
Rumi Deb Bikash Chandra Paul Ramesh Tikekar
A class of general relativistic solutions in isotropic spherical polar coordinates which describe compact stars in hydrostatic equilibrium are discussed. The stellar models obtained here are characterized by four parameters, namely, 𝜆, 𝑘, 𝐴 and 𝑅 of geometrical significance related to the inhomogeneity of the matter content of the star. The stellar models obtained using the solutions are physically viable for a wide range of values of the parameters. The physical features of the compact objects taken up here are studied numerically for a number of admissible values of the parameters. Observational stellar mass data are used to construct suitable models of the compact stars.
Volume 79 Issue 3 September 2012 pp 501-509
Non-adiabatic radiative collapse of a relativistic star under different initial conditions
We examine the role of space-time geometry in the non-adiabatic collapse of a star dissipating energy in the form of radial heat flow, studying its evolution under different initial conditions. The collapse of a star filled with a homogeneous perfect fluid is compared with that of a star filled with inhomogeneous imperfect fluid under anisotropic pressure. Both the configurations are spherically symmetric. However, in the latter case, the physical space 𝑡 = constant of the configurations endowed with spheroidal or pseudospheroidal geometry is assumed to be inhomogeneous. It is observed that as long as the collapse is shear-free, its evolution depends only on the mass and size of the star at the onset of collapse.
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