Junction conditions for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>F</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>gravity and their consequences

Senovilla, José M. M.

doi:10.1103/physrevd.88.064015

Cited by 161 publications

(272 citation statements)

References 34 publications

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“…Besides the continuity of the first fundamental form h μν across the shell, in F(R) theories there exists an additional condition [46], which is [K μ μ ] = 0. If F (R) = 0 (the prime applied to F(R) represents the derivative with respect to R), a third condition is also required [46]: the continuity of R across the surface , i.e.…”

Section: Wormhole Constructionmentioning

confidence: 99%

“…However, quadratic F(R) = R + α R 2 , for which F (R) = 0, allows for the discontinuity of R. In our construction [R] = 0 is automatically fulfilled, because the geometries at both sides of the throat are the same. The field equations on in the case F (R) = 0 have the form [46] …”

Section: Wormhole Constructionmentioning

confidence: 99%

“…If F (R) = 0 (the prime applied to F(R) represents the derivative with respect to R), a third condition is also required [46]: the continuity of R across the surface , i.e.…”

Section: Wormhole Constructionmentioning

confidence: 99%

“…In quadratic F(R), besides the standard energy-momentum tensor S μν , the shell has an external energy flux vector T μ , an external scalar pressure/tension T , and a double layer energy-momentum contribution T μν of Dirac "delta prime" type, resembling classical dipole distributions [46]. All of them are necessary in order to make the complete energy-momentum tensor divergence-free, so that it is locally conserved [46]. But all these contributions are proportional to [R], so in our case they are all zero.…”

Section: Wormhole Constructionmentioning

confidence: 99%

“…They are also useful for the study of thin layers of matter and in braneworld cosmology. In the last decade, the junction conditions have been generalized to F(R) theories of gravity [45,46]. The junction conditions are more stringent in F(R) gravity than in General Relativity.…”

Section: Introductionmentioning

confidence: 99%

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Thin-shell wormholes with charge in F(R) gravity

Eiroa

Figueroa-Aguirre

2016

Eur. Phys. J. C

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In this article, we construct a class of constant curvature and spherically symmetric thin-shell Lorentzian wormholes in F(R) theories of gravity and we analyze their stability under perturbations preserving the symmetry. We find that the junction conditions determine the equation of state of the matter at the throat. As a particular case, we consider configurations with mass and charge. We obtain that stable static solutions are possible for suitable values of the parameters of the model.

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Section: Wormhole Constructionmentioning

confidence: 99%

Section: Wormhole Constructionmentioning

confidence: 99%

“…If F (R) = 0 (the prime applied to F(R) represents the derivative with respect to R), a third condition is also required [46]: the continuity of R across the surface , i.e.…”

Section: Wormhole Constructionmentioning

confidence: 99%

Section: Wormhole Constructionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Thin-shell wormholes with charge in F(R) gravity

Eiroa

Figueroa-Aguirre

2016

Eur. Phys. J. C

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Collapsing Shear‐Free Anisotropic Embedding Star Model in f(R)$f(R)$ Gravity

Nazar,

Abbas,

Abbas

et al. 2024

Fortschritte der Physik

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The current paper studied the dynamics of shear‐free and spherically symmetric collapsing stars by incorporating the features of anisotropic dissipative fluid in the realm of gravity. A complete radiative star model that describes the early static configuration obeying the embedding class 1 approach is generated. To acquittance the exact solutions of the geometric variables, a specific form of pressure anisotropy along with a time‐dependent Karmarkar condition is employed, leading to a spacetime solution that seems to be potentially reliable and regular throughout the collapse process. The matching conditions have been thoroughly investigated between the interior geometry and the Vaidya outgoing solution over the junction interface. The physical attributes of our solutions to the Einstein field equations under two viable and cosmologically well‐consistent models of are manifested. The presented features are in a stable equilibrium state and sustainable to model a dynamic structure of gravitational collapse without forming the black hole.

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Equations for general shells

Senovilla

2018

J. High Energ. Phys.

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The complete set of (field) equations for shells of arbitrary, even changing, causal character are derived in arbitrary dimension. New equations that seem to have never been considered in the literature emerge, even in the traditional cases of everywhere non-null, or everywhere null, shells. In the latter case there arise field equations for some degrees of freedom encoded exclusively in the distributional part of the Weyl tensor. For non-null shells the standard Israel equations are recovered but not only, the additional relations containing also relevant information. The results are applicable to a widespread literature on domain walls, branes and braneworlds, gravitational layers, impulsive gravitational waves, and the like. Moreover, they are of a geometric nature, and thus they can be used in any theory based on a Lorentzian manifold.In [29], the questions of the junction conditions and of the existence of thin shells supported on hypersurfaces of arbitrary, even changing, causal character were addressed. Such hypersurfaces or shells are called general. The importance of dealing with hypersurfaces with possibly changing signature resides in the fact that they actually appear in many physical situations. Furthermore, because they are the generic type of hypersurface in any given spacetime. Some examples of relevant general hypersurfaces are, for instance, the spherically symmetric apparent horizon in Vaidya's spacetime -if the radiation stops at some times; more generally, dynamical horizons which eventually merge with the event horizon in asymptotically flat black-hole spacetimes; any achronal boundary, that is to say, the boundary of any future set [16]; Kerr's stationary limit surface, which is timelike everywhere but tangent to the event horizon at two lines intersecting the axis of symmetry, where it is null [16,48]; the interfaces arising in phase transitions if they occur in a concentrated spatial region and then propagate causally; signature changing braneworlds; and there are many others.Thus, for instance, if one wished to analyze the possibility of placing a surface layer on the stationary limit surface of a Kerr black hole, this should be done on a general, signaturechanging, hypersurface. Similarly, descriptions of signature change in the brane scenario -if we happen to live in a brane of a higher-dimensional world-are described by general shells, see [30,31,32]. The case of achronal boundaries is of particular interest because intuitive arguments lead to the expectation that an initial value problem for the gravitational field equations on such boundaries is well posed, see the interesting discussion in [27]. In addition to the above, a unifying framework for all type of shells, independently of their causal character, is desirable, and this may be achieved by describing general shells.The purpose of this paper is triple: (i) to find the full set of equations for general shells, (ii) to do it in arbitrary spacetime dimension, and (iii) the completion of known results for constant-signature shell...

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Junction conditions forF(R)gravity and their consequences

Cited by 161 publications

References 34 publications

Thin-shell wormholes with charge in F(R) gravity

Thin-shell wormholes with charge in F(R) gravity

Collapsing Shear‐Free Anisotropic Embedding Star Model in f(R)$f(R)$ Gravity

Equations for general shells

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