Dissipative collapse of a Karmarkar star

Abstract

In this paper, we employ the Karmarkar condition to model a spherically symmetric radiating star undergoing dissipative gravitational collapse within the framework of classical general relativity. The collapse ensues from an initial static core satisfying the Karmarkar condition in isotropic coordinates and proceeds nonadiabatically by emitting energy in the form of a radial heat flux to the exterior Vaidya spacetime. We show that the dynamical nature of the collapse is sensitive to the initial static configuration that inherently links the embedding to the final remnant. Our model considered several physical tests on how an initially static stellar structure onset to a radiative collapse.

Radiating composite stars with electromagnetic fields

“…Some recent examples of charged static stars and their interesting properties are given in [1][2][3][4][5][6]. In radiating stars, the radial pressure at the stellar boundary is nonvanishing [7][8][9][10]. As a result, in the modeling of a charged radiating stellar structure, an additional differential equation has to be solved, in addition to the field equations.…”

Model of compact star with ordinary and dark matter

“…This approach is also relevant in the modelling of dark matter in the rotational curves galaxies with color-flavor-locked CFL distributions. As demonstrated in Singh et al (2020a), Govender et al (2020 and Singh et al (2020b) the embedding approach also produces physically acceptable results with relevant equations of state.…”

Gravitationally collapsing stars in f(R) gravity

“…For the solution, we use the Karmarkar condition [51][52][53]. These conditions determine gravitational potentials for static and non-static systems [54][55][56][57]. We must mention here that similar studies on f (R) gravity have been carried out in [41].…”