Radiating star, shear-free gravitational collapse without horizon

Tewari, B. C.; Charan, Kali

doi:10.1007/s10509-014-1851-9

Cited by 23 publications

(12 citation statements)

References 40 publications

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“…For collapsing configurations we must have ( ) 0 f t ≤  . From Equation 29 The new parametric class of solutions of Equation 26 ; we rediscover the Schwarzschild interior solution and the collapsing radiating star model in this case has been studied by de Oliveira et al [13] and Bonnor et al [14] and for n = −1, the solution reduces to Banerjee et al [15], for 3 2, 2 n = − − , it reduces to Tewari [19] [20], for 1 2 n =− − , horizon-free case studied by Tewari and Charan [21]. We here present some more special solutions and a detailed study of a class of solutions.…”

Section: Solution Of the Field Equationsmentioning

confidence: 99%

“…Santos [10] studied the junction conditions of collapsing spherically symmetric shear-free non-adiabatic fluid with radial heat flow which was based on relativistic models suggested by Glass [11]. On the similar ground a number of stellar models (Maiti [12], de Oliveira et al [13], Bonnor et al [14], Banerjee et al [15], Herrera et al [16], Tewari [17]- [20], Tewari and Charan [21], Sharma and Tikekar [22], Ivanov [23], Pinheiro and Chan [24] and also references therein) have been reported with the impact of various factors such as shear, inhomogeneity, anisotropy, electromagnetic field and various dissipative processes on the evolution.…”

Section: Introductionmentioning

confidence: 99%

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Dissipative Spherical Gravitational Collapse of Isotropic Fluid

Tewari¹,

Charan²

2015

JMP

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We present a number of parametric class of exact solutions of a radiating star and the matching conditions required for the description of physically meaningful fluid. A number of previously known class of solutions have been rediscovered which describe well behaved nature of fluid distributions. The interior matter fluid is shear-free spherically symmetric isotropic and undergoing radial heat flow. The interior metric obeyed all the relevant physical and thermodynamic conditions and matched with Vaidya exterior metric over the boundary. Initially the interior solutions represent a static configuration of perfect fluid which then gradually starts evolving into radiating collapse. The apparent luminosity as observed by the distant observer at rest at infinity and the effective surface temperature are zero in remote past at the instant when collapse begins and at the stage when collapsing configuration reaches the horizon of the black hole.

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Section: Solution Of the Field Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Dissipative Spherical Gravitational Collapse of Isotropic Fluid

Tewari¹,

Charan²

2015

JMP

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“…For different values of n or l Equations (22) and 23give a variety of solutions and they are categorized as isotropic pressure and homogeneous density, isotropic pressure and inhomogeneous density while some inhomogeneous density and anisotropic pressure. For 0 = n we get the homogeneous density and anisotropic pressure, for 1 = − n we get the isotropic pressure and homogeneous density and in this case solution reduces to Banerjee et al [38] and for 1 = n we get isotropic pressure and inhomogeneous density.…”

Section: The New Parametric Class Of Solution and Some Proposed Solutmentioning

confidence: 99%

“…The prominent work in pure radiation is due to Tewari and he solved the Einstein's field equations with a new approach and developed the Quasar models [10]- [13]. While a number of realistic models in diffusion approximation with the impact of various factors such as inhomogeneity, anisotropy, viscosity, electromagnetic field and various dissipative processes on the evolution are critically discussed by de Oliveira et al [14]; Bonnor et al [15]; Herrera et al [16]; Maharaj and Govender [17]; Ivanov [18]; Tewari [19] [20]; Pinheiro and Chan [21]; Tewari and Charan [22] [23]; Sharif and Iftikhar [24].…”

Section: Introductionmentioning

confidence: 99%

Spherical Gravitational Collapse of Anisotropic Radiating Fluid Sphere

Tewari¹,

Charan²,

Rani³

2016

IJAA

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We here present a relativistic model for a spherically symmetric anisotropic fluid to study the various factors of physical and thermal phenomenon during the evolution of a collapsing star dissipating energy in the form of radial heat flow. We also proposed a table of some new parametric class of solutions which will be useful for constructing the new compact star models. The constructed algorithm obeys all the relevant requirements of a realistic model and matched with Vaidya exterior metric over the boundary. At the initial stage the interior solutions represent a static configuration of perfect fluid which then gradually starts evolving into radiating collapse. The apparent luminosity as observed by the distant observer at rest at infinity and the effective surface temperature are zero in remote past at the instant when collapse begins and at the stage when collapsing configuration reaches the horizon of the black hole.

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“…They found that the objects do not achieve the end state of being a black hole; instead, the presence of charge results in the formation of naked singularity [28]. The naked singularity is a hypothetical singularity without an event horizon [29,30]. The event horizon is the boundary of a black hole.…”

Section: Introductionmentioning

confidence: 99%

Charged anisotropic spherical collapse with heat flow

2021

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In this article, we study the shear-free gravitational collapse of a charged radiating star. The Einstein field equations of gravitational collapse for the charged stars are known to give rise to a high degree of non-linearity in the ordinary differential equation coming from junction conditions. The attempts to solve it analytically proved to be unfortunate. Numerical methods have been suggested in the past. However, the high degree of non-linearity tends to introduce fluctuations and large round off errors in the numerical calculation. A new ansatz is proposed in the present work to reduce the degree of non-linearity. An ordinary differential equation is derived by satisfying junction conditions, and its numerical solution is demonstrated. Physical quantities associated with the collapse process are plotted to observe the effect of charge on these quantities. It is concluded that the charge can delay the collapse of a star and can even prevent it depending upon the amount of charge. It is also verified that the solution satisfies all the energy conditions.

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Radiating star, shear-free gravitational collapse without horizon

Cited by 23 publications

References 40 publications

Dissipative Spherical Gravitational Collapse of Isotropic Fluid

Dissipative Spherical Gravitational Collapse of Isotropic Fluid

Spherical Gravitational Collapse of Anisotropic Radiating Fluid Sphere

Charged anisotropic spherical collapse with heat flow

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