Dynamical instability for radiating anisotropic collapse

We present a complete set of the equations and matching conditions required for the description of physically meaningful charged, dissipative, spherically symmetric gravitational collapse with shear. Dissipation is described with both free-streaming and diffusion approximations. The effects of viscosity are also taken into account. The roles of different terms in the dynamical equation are analyzed in detail. The dynamical equation is coupled to a causal transport equation in the context of Israel-Stewart theory. The decrease of the inertial mass density of the fluid, by a factor which depends on its internal thermodynamic state, is reobtained, with the viscosity terms included. In accordance with the equivalence principle, the same decrease factor is obtained for the gravitational force term. The effect of the electric charge on the relation between the Weyl tensor and the inhomogeneity of energy density is discussed.2

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“…The components (60)(61)(62)(63)(64) can be written in terms of the Einstein tensor G αβ = R αβ − g αβ R/2 and the mass function (25) producing…”

Section: Discussionmentioning

confidence: 99%

“…which is just the generalization of the Tolman-Oppenheimer-Volkov equation for anisotropic charged fluids obtained in [62] while studying dynamical instability for radiating anisotropic collapse. When the static fluid reduces to charged dust, with P r = P ⊥ = 0, then, by using (15), (43) becomes…”

Section: Static Charged Dustmentioning

confidence: 99%

Nonadiabatic charged spherical gravitational collapse

et al. 2007

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“…A pioneer work in this direction was done by Chandrasekhar (Chandrasekhar 1964). Afterwards, this issue has been investigated by many authors for adiabatic, non-adiabatic, anisotropic and shearing viscous fluids (Herrera et al 1989;Chan et al 1989;Chan et al 1994;Chan et al 1993;Herrera et al, arXiv/1010.1518. The dynamical instability of collapsing fluids can be well discussed in term of adiabatic index Γ.…”

Section: Introductionmentioning

confidence: 99%

Newtonian and post Newtonian expansionfree fluid evolution in f(R) gravity

Sharif¹,

Kausar²

2011

Astrophys Space Sci

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We consider a collapsing sphere and discuss its evolution under the vanishing expansion scalar in the framework of f (R) gravity. The fluid is assumed to be locally anisotropic which evolves adiabatically. To study the dynamics of the collapsing fluid, Newtonian and post Newtonian regimes are taken into account. The field equations are investigated for a well-known f (R) model of the form R + δR 2 admitting Schwarzschild solution. The perturbation scheme is used on the dynamical equations to explore the instability conditions of expansionfree fluid evolution. We conclude that instability conditions depend upon pressure anisotropy, energy density and some constraints arising from this theory.

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“…The dynamics of self-gravitating object during collapse process has been analyzed in GR (Skripkin 1960;Chandrasekhar 1964;Herrera, Santos & Le Denmat 1989;Chan, Herrera & Santos 1993;Herrera & Santos 1995;Herrera, Le Denmat and Santos & 2012) and modified theories of gravity such as f (R), f (R, T ), Brans-Dicke, Einstein Gauss-Bonnet gravity in spherical as well as cylindrical symmetry (Sharif & Manzoor 2014,2015Kausar, Noureen & Shahzad 2015;Kausar 2013) while in f (T ) gravity for spherical symmetry , 2015. The disturbance in hydrostatic equilibrium of a stellar object leads to the collapse process.…”

Section: Introductionmentioning

confidence: 99%

Dynamical instability of cylindrical symmetric collapsing star in generalized teleparallel gravity

Jawad

Momeni

Rani

et al. 2016

Astrophys Space Sci

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This paper is devoted to analyze the dynamical instability of a self-gravitating object undergoes to collapse process. We take the framework of generalized teleparallel gravity with cylindrical symmetric gravitating object. The matter distribution is represented by locally anisotropic energy-momentum tensor. We develop basic equations such as dynamical equations along with matching conditions and Harrison-Wheeler equation of state. By applying linear perturbation strategy, we construct collapse equation which is used to accomplish the instability ranges in Newtonian and post-Newtonian regimes. We find these ranges for isotropic pressure as well as reduce the results in general relativity. The unstable behavior depends on matter, metric, mass and torsion based terms. *

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Dynamical instability for radiating anisotropic collapse

Cited by 453 publications

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Nonadiabatic charged spherical gravitational collapse

Nonadiabatic charged spherical gravitational collapse

Newtonian and post Newtonian expansionfree fluid evolution in f(R) gravity

Dynamical instability of cylindrical symmetric collapsing star in generalized teleparallel gravity

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