Singularity formation in radiating star with dark energy background

Abstract

In this paper, we considered the gravitational collapse of a symmetric radiating star consisting of perfect fluid (baryonic) in the background of dark energy (DE) with general equation of state. The effect of DE on the singularity formation has been discussed first separately (only DE present) and then combination of both baryonic and DE interaction. We have also showed that DE components play important role in the formation of Black-Hole(BH). In some cases the collapse of radiating star leads to black hole formation and in other cases it forms Naked-Singularity(or, eternally collapse). The present work is in itself remarkable to describe the effect of dark energy on singularity formation in radiating star.

arXiv commentLast section concluded as- From above table-1 we see that due to the presence of $p_{DE}$, the loss of luminosity increases the when ${\rho }_0>\frac{3R_0^2}{k{r}_{\sum }^2}$ and it slow down for ${\rho }_0<\frac{3R_0^2}{k{r}_{\sum }^2}$. Thus for different value of ${\epsilon }^{{}^{\prime }}$, $p_{DE}$ plays the important role in the formation of black hole

References in corpus (12)

• Phantom Energy and Cosmic Doomsday
• Cosmological Tracking Solutions
• The final state and thermodynamics of dark energy universe
• A classification of scalar field potentials with cosmological scaling solutions
• Black hole mass decreasing due to phantom energy accretion
• On the Role of Initial Data in the Gravitational Collapse of Inhomogeneous Dust
• Initial data and the end state of spherically symmetric gravitational collapse
• Likely formation of general relativistic radiation pressure supported stars or "eternally collapsing objects"
• Problems with Time-Varying Extra Dimensions or "Cardassian Expansion" as Alternatives to Dark Energy
• Black Hole Formation from Collapsing Dust Fluid in a Background of Dark Energy
• Cosmological constant and late transient acceleration of the universe in the Horava-Witten Heterotic M-Theory on S^{1}/Z_{2}
• Scalar field collapse in a conformally flat spacetime