Two-fluid atmosphere for relativistic stars

Glass, E. N.; Krisch, J. P.

doi:10.1088/0264-9381/16/4/007

Cited by 49 publications

(59 citation statements)

References 24 publications

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“…In general, T + ab represents a Type II fluid as defined by Hawking and Ellis [38]. This additional fluid component has also been interpreted by Husain [28], Wang and Wu [29], Glass and Krisch [32,33] and Krisch and Glass [30] as a string fluid distribution in four dimensions. The null vector l is a double null eigenvector of the energy momentum tensor (8) and the vector n is normal to the spatial hypersurface.…”

Section: Constructing the Modelmentioning

confidence: 75%

“…The conditions for physically reasonable energy transport mechanisms in the generalised Vaidya spacetime were explored by Krisch and Glass [30] and Yang [31]. Glass and Krisch [32,33] used the notion of the null fluid to describe the qualitative features of a localised string distribution in four dimensions, and generated analytical solutions for null string fluids exhibiting pressure isotropy in the limit of diffusion. This realisation that a Type II null fluid can be used to describe a diffusing string on cosmological scales, in particular, supports the earlier work of Vilenkin [34], Percival [35] and Percival and Strunz [36].…”

Section: Introductionmentioning

confidence: 99%

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The effect of a two-fluid atmosphere on relativistic stars

2015

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We model the physical behaviour at the surface of a relativistic radiating star in the strong gravity limit. The spacetime in the interior is taken to be spherically symmetrical and shear-free. The heat conduction in the interior of the star is governed by the geodesic motion of fluid particles and a non-vanishing radially directed heat flux. The local atmosphere in the exterior region is a two-component system consisting of standard pressureless (null) radiation and an additional null fluid with non-zero pressure and constant energy density. We analyse the generalised junction condition for the matter and gravitational variables on the stellar surface and generate an exact solution. We investigate the effect of the exterior energy density on the temporal evolution of the radiating fluid pressure, luminosity, gravitational redshift and mass flow at the boundary of the star. The influence of the density on the rate of gravitational collapse is also probed and the strong, dominant and weak energy conditions are also tested. We show that the presence of the additional null fluid has a significant effect on the dynamical evolution of the star.

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Section: Constructing the Modelmentioning

confidence: 75%

Section: Introductionmentioning

confidence: 99%

The effect of a two-fluid atmosphere on relativistic stars

2015

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“…In the framework of the same approach a large class of solutions, including Type II fluids, and which includes most of the known solutions of the Einstein field equations, has been derived, in four dimensions by Wang and Wu [22], and in N ≥ 4 dimensions by Villas da Rocha [23]. The Vaidya radiating metric has been extended to include both a radiation field and a string fluid by Glass and Krisch [24], [25] and by Govinder and Govender [26].…”

Section: Introductionmentioning

confidence: 99%

Gravitational collapse of a Hagedorn fluid in Vaidya geometry

Harkó

2003

Phys. Rev. D

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The gravitational collapse of a high-density null charged matter fluid, satisfying the Hagedorn equation of state, is considered in the framework of the Vaidya geometry. The general solution of the gravitational field equations can be obtained in an exact parametric form. The conditions for the formation of a naked singularity, as a result of the collapse of the compact object, are also investigated. For an appropriate choice of the arbitrary integration functions the null radial outgoing geodesic, originating from the shell focussing central singularity, admits one or more positive roots. Hence a collapsing Hagedorn fluid could end either as a black hole, or as a naked singularity. A possible astrophysical application of the model, to describe the energy source of gamma-ray bursts, is also considered.

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“…If the mass is also a function of retardate time, we find the Vaidya metric of a short-wavelength photons radiation atmosphere in addition to the string fluid [5].…”

Section: Introductionmentioning

confidence: 96%

DILATION DARK MATTER IN VAIDYA–de SITTER SPACETIME

Cristina

1999

Int. J. Mod. Phys. D

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The exterior of a relativistic star can be modelated with the Vaidya radiating metric. It is started from the generalized Vaidya metric that allows a type II fluid and studied the conditions of generating new analytical solutions of the Einstein's field equations. It is shown that the mass parameter solution gives the classical de Sitter universe in the static case and the extended de Sitter metric coupled with a dilation scalar field in the time-dependent case. It is concluded that in the time-dependent case the atmosphere of a relativistic star consists on an anisotropic string fluid coupled with a dark matter null fluid and interpreted the scalar field as the particle that produces the dark matter.

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Two-fluid atmosphere for relativistic stars

Cited by 49 publications

References 24 publications

The effect of a two-fluid atmosphere on relativistic stars

The effect of a two-fluid atmosphere on relativistic stars

Gravitational collapse of a Hagedorn fluid in Vaidya geometry

DILATION DARK MATTER IN VAIDYA–de SITTER SPACETIME

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