ritu tamta - Academia.edu (original) (raw)

Papers by ritu tamta

SAMRIDDHI : A Journal of Physical Sciences, Engineering and Technology

In the present article, we perceive a new kind of mass function to solve Einstein's field equ... more In the present article, we perceive a new kind of mass function to solve Einstein's field equation and generate spherically symmetric models of ultra-dense stellar objects. By assuming a suitable form of mass function, we study the out-march of all physical parameters within the anisotropic fluid spheres. We find that the radial and transverse pressures, the density of matter, redshift, mass function are regular and well behaved inside the compact fluid spheres. Our model is stable under the action of hydrostatic, anisotropic, and gravitational forces and the causality condition is well satisfied inside the fluid spheres. The graphical representation of the adiabatic index reconfirms the stability of our model and the compactness parameter lies within the Buchdahl limit. The newly obtained solution is free from any singularity and satisfies all energy conditions, i.e., strong energy condition, weak energy condition, and null energy condition. We construct models of compact stars...

Journal of Modern Physics, 2017

In the present article, we explore a new static, spherically symmetric charged anisotropic fluid ... more In the present article, we explore a new static, spherically symmetric charged anisotropic fluid model of compact star in curvature coordinates. We consider metric potential 44 g of Durgapal's fifth solution [1] with a specific choice of electric field intensity E and physically acceptable expression of anisotropy factor ∆ , which involve parameters K (charge) and ∆ (anisotropy) respectively. The solution so obtained is utilized to construct the model for super-dense star like neutron star. We have analysed that corresponding to 0.1 X = , 2.8 K = , 1.6 α = and by assuming surface density 14 3 2 10 gm cm b ρ = × , the mass of the compact star comes out to be 2.17M Θ with radius 14.51 kms, which closely resembles to that of PSRJ0348 + 0432. The solution is well behaved for the values of K satisfying 1 5 K ≤ <. Our model is described analytically as well as with the help of graphical representations. Our solution is well behaved and free from any central singularity. It also satisfies all the energy conditions as well as the causality condition thus reconfirming the stability of our model.

Modern Physics Letters A, 2019

In this paper, we searched two new exact solutions of Einstein’s field equations for modeling of ... more In this paper, we searched two new exact solutions of Einstein’s field equations for modeling of compact cold stars using embedded class one spacetime continuum. We find out the expressions for pressure, density, anisotropy, redshift, metric potentials and other physical variables in terms of algebraic and trigonometric expressions and observe that all variables show well-behaved trends inside the compact stellar configurations. The causality condition is well maintained by our stellar models, i.e. the radial velocity and transverse velocity are less than l. The stability of our models is assessed via different stability criteria. The Buchdahl condition holds good for our solution. Herrera’s cracking method is applied to check the stability of stellar models. We generate anisotropic compact star models, whose masses and radii are in close agreement with the observed values for compact stars 4U 1538-52, LMCX-4, PSRJ1614-2230. A comparative analysis of the proposed models is carried o...

SAMRIDDHI : A Journal of Physical Sciences, Engineering and Technology

In the present article, we perceive a new kind of mass function to solve Einstein's field equ... more In the present article, we perceive a new kind of mass function to solve Einstein's field equation and generate spherically symmetric models of ultra-dense stellar objects. By assuming a suitable form of mass function, we study the out-march of all physical parameters within the anisotropic fluid spheres. We find that the radial and transverse pressures, the density of matter, redshift, mass function are regular and well behaved inside the compact fluid spheres. Our model is stable under the action of hydrostatic, anisotropic, and gravitational forces and the causality condition is well satisfied inside the fluid spheres. The graphical representation of the adiabatic index reconfirms the stability of our model and the compactness parameter lies within the Buchdahl limit. The newly obtained solution is free from any singularity and satisfies all energy conditions, i.e., strong energy condition, weak energy condition, and null energy condition. We construct models of compact stars...

Journal of Modern Physics, 2017

In the present article, we explore a new static, spherically symmetric charged anisotropic fluid ... more In the present article, we explore a new static, spherically symmetric charged anisotropic fluid model of compact star in curvature coordinates. We consider metric potential 44 g of Durgapal's fifth solution [1] with a specific choice of electric field intensity E and physically acceptable expression of anisotropy factor ∆ , which involve parameters K (charge) and ∆ (anisotropy) respectively. The solution so obtained is utilized to construct the model for super-dense star like neutron star. We have analysed that corresponding to 0.1 X = , 2.8 K = , 1.6 α = and by assuming surface density 14 3 2 10 gm cm b ρ = × , the mass of the compact star comes out to be 2.17M Θ with radius 14.51 kms, which closely resembles to that of PSRJ0348 + 0432. The solution is well behaved for the values of K satisfying 1 5 K ≤ <. Our model is described analytically as well as with the help of graphical representations. Our solution is well behaved and free from any central singularity. It also satisfies all the energy conditions as well as the causality condition thus reconfirming the stability of our model.

Modern Physics Letters A, 2019

In this paper, we searched two new exact solutions of Einstein’s field equations for modeling of ... more In this paper, we searched two new exact solutions of Einstein’s field equations for modeling of compact cold stars using embedded class one spacetime continuum. We find out the expressions for pressure, density, anisotropy, redshift, metric potentials and other physical variables in terms of algebraic and trigonometric expressions and observe that all variables show well-behaved trends inside the compact stellar configurations. The causality condition is well maintained by our stellar models, i.e. the radial velocity and transverse velocity are less than l. The stability of our models is assessed via different stability criteria. The Buchdahl condition holds good for our solution. Herrera’s cracking method is applied to check the stability of stellar models. We generate anisotropic compact star models, whose masses and radii are in close agreement with the observed values for compact stars 4U 1538-52, LMCX-4, PSRJ1614-2230. A comparative analysis of the proposed models is carried o...