Embedding with Vaidya geometry

Николаев, А. В.; Maharaj, S. D.

doi:10.1140/epjc/s10052-020-8231-0

Cited by 12 publications

(9 citation statements)

References 57 publications

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“…Comparing ∂ρ s ∂v in the above result (27) with the heat equation (24) (where n is replaced by ρ s ), we have, after some algebraic manipulation…”

Section: Derivation Of the Diffusion Equationmentioning

confidence: 99%

“…These results for type I or type II (or combinations of the two) fluids have proven fruitful in stellar modeling, both in general relativity and EGB gravity. A recent paper by Nikolaev and Maharaj [27] showed that the generalised Vaidya spacetime may be embedded in higher dimensional Euclidean spaces. This opens avenues for further astrophysical research in modified gravity theories.…”

Section: Introductionmentioning

confidence: 99%

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Generalised radiating fields in Einstein–Gauss–Bonnet gravity

Brassel

Maharaj

2020

Eur. Phys. J. C

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A five-dimensional spherically symmetric generalised radiating field is studied in Einstein–Gauss–Bonnet gravity. We assume the matter distribution is an extended Vaidya-like source and the resulting Einstein–Gauss–Bonnet field equations are solved for the matter variables and mass function. The evolution of the mass, energy density and pressure are then studied within the spacetime manifold. The effects of the higher order curvature corrections of Einstein–Gauss–Bonnet gravity are prevalent in the analysis of the mass function when compared to general relativity. The effects of diffusive transport are then considered and we derive the specific equation for which diffusive behaviour is possible. Gravitational collapse is then considered and we show that collapse ends with a weak and conical singularity for the generalised source, which is not the case in Einstein gravity.

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“…Comparing ∂ρ s ∂v in the above result (27) with the heat equation (24) (where n is replaced by ρ s ), we have, after some algebraic manipulation…”

Section: Derivation Of the Diffusion Equationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Generalised radiating fields in Einstein–Gauss–Bonnet gravity

Brassel

Maharaj

2020

Eur. Phys. J. C

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“…subject to R 2323 = 0 [55]. It ought to be noticed that all the components are given in (31) fulfill the Codazzi equation (28). Moreover, there is a significant point that we might want to refer to: for an overall spherically symmetric space-time, its symmetric tensor b ij can be composed as follows…”

Section: Basic Formulation Of Class One Condition and Its Solution In...mentioning

confidence: 99%

Charged anisotropic strange stars in Brans-Dicke gravity with a massive scalar field through embedding approach

Maurya¹,

Singh²,

Govender³

et al. 2020

Preprint

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In this exposition we seek solutions of the Einstein-Maxwell field equations in the presence of a massive scalar field cast in the Brans-Dicke (BD) formalism which describe charged anisotropic strange stars. The interior spacetime is described by a spherically symmetric static metric of embedding class I. This reduces the problem to a single-generating function of the metric potential which is chosen by appealing to physics based on regularity at each interior point of the stellar interior. The resulting model is subjected to rigorous physical checks based on stability, causality and regularity. We show that our solutions describe compact objects such as PSR J1903+327; Cen X-3; EXO 1785-248 & LMC X-4 to an excellent approximation. Novel results of our investigation reveal that the scalar field leads to higher surface charge densities which in turn affects the compactness and upper and lower values imposed by the modified Buchdahl limit for charged stars. Our results also show that the electric field and scalar field which originate from entirely different sources couple to alter physical characteristics such as mass-radius relation and surface redshift of compact objects. This superposition of the electric and scalar fields is enhanced by an increase in the BD coupling constant, ωBD.

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“…The embedding of the generalized Vaidya (GV) solution via the Karmarkar solution shows that embedding does not allow the interpretation of the generalized Vaidya spacetime as a diffusive medium. In other words, the Karmarkar condition prohibits the GV solution to be interpreted as an atmosphere composed of radiation and diffusive strings of a star undergoing dissipative collapse in the form of a radial heat flux [31]. The Karmarkar condition has been extended to incorporate time-dependent systems which include modelling shear-free, dissipative collapse [32][33][34][35].…”

Section: Introductionmentioning

confidence: 99%

“…(31), we found the following relationship in terms of the Riemann componentsR 0202 R 1313 = R 0101 R 2323 , (32)subject to R 2323 = 0 (Pandey and Sharma condition[63]). It ought to be noticed that all the components are given in(31) fulfill the Codazzi equation(28). On the other hand, in the case of a general non-static spherically symmetric spacetime, the relation between components for symmetric tensor b i j and Riemann tensor R i jhk can be given as followsb 01 b 22 = R 1212 and b 00 b 11 − (b 01 ) 2 = R 0101 , (…”

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confidence: 99%

Anisotropic stars via embedding approach in Brans–Dicke gravity

et al. 2021

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In the present article, the solution of the Einstein–Maxwell field equations in the presence of a massive scalar field under the Brans-Dicke (BD) gravity is obtained via embedding approach, which describes a charged anisotropic strange star model. The interior spacetime is described by a spherically symmetric static metric of embedding class I. This reduces the problem to a single-generating function of the metric potential which is chosen by appealing to physics based on regularity at each interior point of the stellar interior. The resulting model is subjected to rigorous physical checks based on stability, causality and regularity for particular object PSR J1903+327. We also show that our solutions describe compact objects such as PSR J1903+327; Cen X-3; EXO 1785-248 and LMC X-4 to an excellent approximation. Novel results of our investigation reveal that the scalar field leads to higher surface charge densities which in turn affects the compactness and upper and lower values imposed by the modified Buchdahl limit for charged stars. Our results also show that the electric field and scalar field which originate from entirely different sources couple to alter physical characteristics such as mass-radius relation and surface redshift of compact objects. This superposition of the electric and scalar fields is enhanced by an increase in the BD coupling constant, $$\omega _{BD}$$ ω BD .

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Embedding with Vaidya geometry

Cited by 12 publications

References 57 publications

Generalised radiating fields in Einstein–Gauss–Bonnet gravity

Generalised radiating fields in Einstein–Gauss–Bonnet gravity

Charged anisotropic strange stars in Brans-Dicke gravity with a massive scalar field through embedding approach

Anisotropic stars via embedding approach in Brans–Dicke gravity

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