Minimal geometric deformation of Yang-Mills-Dirac stellar configurations

Rocha, Roldão da

doi:10.1103/physrevd.102.024011

Cited by 52 publications

(32 citation statements)

References 79 publications

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“…where c is an arbitrary scaling factor for the time coordinate, chosen such that it matches with the proper time for a remote observer, that is, lim r→∞ h(r) = 1. Then, substituting (20) in the field Equations ( 18) and ( 19), one can express the coefficients h i , f i i ≥ 2 in terms of the free parameters r 0 and f 1 , so that…”

Section: Einstein-weyl Gravitymentioning

confidence: 99%

“…and similarly for the remaining coefficients. Fixing the horizon radius r 0 and using the above expansions (20) to obtain the initial data at r i (where r i is taken to be very close to the horizon radius r 0 ), the field Equations ( 18) and ( 19) can be numerically integrated by starting the integration at the distance r i . The shooting method is used in order to find the appropriate values of the parameters c and f 1 in (20) such that the solution is asymptotically flat up to a large distance of r = r f ∼ 40r i .…”

Section: Einstein-weyl Gravitymentioning

confidence: 99%

“…The method was later extended to investigate new black hole solutions [10,11] and to generate physically meaningful interior stellar solutions [12] (for some other more recent applications see Refs. [13][14][15][16][17][18][19][20][21]). Gravitational decoupling has also been studied in modified theories of gravity such as f (R, T) [22,23], Gauss-Bonnet gravity [24], f (G) gravity [25] and Rastall gravity [26].…”

Section: Introductionmentioning

confidence: 99%

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Gravitational Decoupling in Higher Order Theories

Sultana

2021

Symmetry

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Gravitational decoupling via the Minimal Geometric Deformation (MGD) approach has been used extensively in General Relativity (GR), mainly as a simple method for generating exact anisotropic solutions from perfect fluid seed solutions. Recently this method has also been used to generate exact spherically symmetric solutions of the Einstein-scalar system from the Schwarzschild vacuum metric. This was then used to investigate the effect of scalar fields on the Schwarzschild black hole solution. We show that this method can be extended to higher order theories. In particular, we consider fourth order Einstein–Weyl gravity, and in this case by using the Schwarzschild metric as a seed solution to the associated vacuum field equations, we apply the MGD method to generate a solution to the Einstein–Weyl scalar theory representing a hairy black hole solution. This solution is expressed in terms of a series using the Homotopy Analysis Method (HAM).

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Section: Einstein-weyl Gravitymentioning

confidence: 99%

Section: Einstein-weyl Gravitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Gravitational Decoupling in Higher Order Theories

Sultana

2021

Symmetry

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“…MGD-decoupling methods represent a realistic algorithm to derive and scrutinize compact stars. The finite brane tension drives the ways to deform the Schwarzschild solution of the Einstein's effective field equations [14][15][16][17][18][19]. The cosmic microwave background anisotropy, observed by the Wilkinson Microwave Anisotropy Probe, rules the fluid brane tension to attain finite values and to vary according to the temperature across a cosmological time scale [20][21][22], emulating Eötvös fluid membranes [23].…”

Section: Introductionmentioning

confidence: 99%

Gravitational decoupling and superfluid stars

Rocha

2021

Eur. Phys. J. C

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The gravitational decoupling is applied to studying minimal geometric deformed (MGD) compact superfluid stars, in covariant logarithmic scalar gravity on fluid branes. The brane finite tension is shown to provide more realistic values for the asymptotic value of the mass function of MGD superfluid stars, besides constraining the range of the self-interacting scalar field, minimally coupled to gravity. Several other physical features of MGD superfluid stars, regulated by the finite brane tension and a decoupling parameter, are derived and discussed, with important corrections to the general-relativistic limit that corroborate to current observational data.

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“…Interestingly, recently a simple, powerful and versatile tool denominated gravitational decoupling by minimal geometric deformation (MGD) [78][79][80][81][82][83][84][85][86][87][88] was developed to introduce anisotropic behavior into the matter distribution, describing a wide range of solutions within the framework of Einstein gravity theory and beyond it . In this connection, some pioneering works on MGD have been done by da Rocha and his collaborators in different aspects [113][114][115][116][117][118]. Furthermore, the inverse problem i.e., given a minimally deformed and anisotropic space-time: what is its non-deformed and isotropic counterpart?…”

Section: Introductionmentioning

confidence: 99%

An EGD model in the background of embedding class I space–time

2020

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This work is devoted to the study of relativistic anisotropic compact objects. To obtain this class of solutions of the Einstein field equations, we have developed a general scheme to generate the metric of the space–time describing the interior of the compact structure. This approach is based on the class I space–time and the extended gravitational decoupling by means of an extended geometric deformation (EGD). The class I condition provides a differential equation relating both metric potential $$\nu $$ ν and $$\lambda $$ λ , whilst the EGD translates the metric potentials to $$ \nu =\xi +\beta \,h(r)$$ ν = ξ + β h ( r ) and $$ \lambda =-\ln [\mu +\beta \,f(r)]$$ λ = - ln [ μ + β f ( r ) ] , where h(r) and f(r) are the deformation functions and $$\beta $$ β a dimensionless constant. In this case the pair $$\{\xi ,\mu \}$$ { ξ , μ } represents the seed solution satisfying the class I condition without any deformation. Once the deformed metric potentials are inserted into the class I, the main task is to obtain h(r) or f(r). So, in this case a particular ansatz for h(r) is considered in conjunction with $$\beta =0.5$$ β = 0.5 to get f(r). In order to check feasibility of our model, we have performed a thoroughly physical, mathematical and graphical analysis.

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Minimal geometric deformation of Yang-Mills-Dirac stellar configurations

Cited by 52 publications

References 79 publications

Gravitational Decoupling in Higher Order Theories

Gravitational Decoupling in Higher Order Theories

Gravitational decoupling and superfluid stars

An EGD model in the background of embedding class I space–time

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