Large scale structures and the cubic galileon model

Bhattacharya, Sourav; Dialektopoulos, Konstantinos F.; Tomaras, T.N.

doi:10.1088/1475-7516/2016/05/036

Cited by 24 publications

(23 citation statements)

References 63 publications

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“…Since, to first order in φ N , the Hawking-Hayward mass is gaugeindependent, this result is manifestly gauge-invariant to this order although it is derived using the conformal Newtonian gauge (23). 1 The mass (25) can also be calculated directly from the post-FLRW metric (23), obtaining the same result [23].…”

Section: Hawking-hayward Mass In a Perturbed Flrw Cosmosmentioning

confidence: 95%

“…(26), the correction −φ N R (HR) 2 is neglected for structures of size R much smaller than the Hubble radius (this term is of second order in R/H −1 ). The current literature on the turnaround radius is restricted to this spherical situation [12][13][14][15][24][25][26][27][28][29][30][31]. In this context, the turnaround radius is obtained when the "local" and the "cosmological" contributions to the right hand side of Eq.…”

Section: Turnaround Size Of a Large Structurementioning

confidence: 99%

“…The turnaround radius has been discussed also in alternative theories of gravity (see e.g. [24][25][26][27][28][29][30][31]), but in this work we focus solely on the standard GR picture. Thus far, the literature on the turnaround radius has studied only spherical structures.…”

Section: Introductionmentioning

confidence: 99%

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Turnaround size of non-spherical structures

Giusti

Faraoni

2019

Physics of the Dark Universe

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The turnaround radius of a large structure in an accelerating universe has been studied only for spherical structures, while real astronomical systems deviate from spherical symmetry. We show that, for small deviations from spherical symmetry, the gauge-invariant characterization of the turnaround size using the Hawking-Hayward quasi-local mass and spherical symmetry still applies, to first order in the cosmological perturbation potentials and in the deviations from sphericity. This is the first step to include non-spherical systems in the physics of turnaround. *

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Section: Hawking-hayward Mass In a Perturbed Flrw Cosmosmentioning

confidence: 95%

Section: Turnaround Size Of a Large Structurementioning

confidence: 99%

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Turnaround size of non-spherical structures

Giusti

Faraoni

2019

Physics of the Dark Universe

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“…Since its proposal, the maximum turn around radius as a useful cosmological observable has received considerable attention in the context of modified or alternative gravity/dark energy models [31][32][33][34][35][36][37]. The goal is of course to constrain the additional parameters of such theories.…”

Section: Introduction and Overviewmentioning

confidence: 99%

“…For example, for a McVittie space-time [38][39][40] a derivation of the turn around radius can be found in [31][32][33], by analyzing geodesics and also using the quasilocal mass function of [41,42]. In [34] a constraint on the matter-galileon coupling parameter was obtained for a cubic galileon model [43]. Both an upper and a lower bound were obtained for this coupling.…”

Section: Introduction and Overviewmentioning

confidence: 99%

Cosmic structure sizes in generic dark energy models

Bhattacharya

Tomaras

2017

Eur. Phys. J. C

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The maximum allowable size of a spherical cosmic structure as a function of its mass is determined by the maximum turn around radius R TA,max , the distance from its center where the attraction on a radial test particle due to the spherical mass is balanced with the repulsion due to the ambient dark energy. In this work, we extend the existing results in several directions. (a) We first show that, for w = −1, the expression for R TA,max found earlier, using the cosmological perturbation theory, can be derived using a static geometry as well. (b) In the generic dark energy model with arbitrary time dependent state parameter w(t), taking into account the effect of inhomogeneities upon the dark energy as well, it is shown that the data constrain w(t = today) > −2.3. (c) We address the quintessence and the generalized Chaplygin gas models, both of which are shown to predict structure sizes consistent with observations.

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On the stability of cubic galileon accretion

Bergliaffa

Maier

2017

Annals of Physics

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We examine the stability of steady-state galileon accretion for the case of a Schwarzshild black hole. Considering the galileon action up to the cubic term in a static and spherically symmetric background we obtain the general solution for the equation of motion which is divided in two branches. By perturbing this solution we define an effective metric which determines the propagation of fluctuations. In this general picture we establish the position of the sonic horizon together with the matching condition of the two branches on it. Restricting to the case of a Schwarzschild background, we show, via the analysis of the energy of the perturbations and its time derivative, that the accreting field is linearly stable.

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Large scale structures and the cubic galileon model

Cited by 24 publications

References 63 publications

Turnaround size of non-spherical structures

Turnaround size of non-spherical structures

Cosmic structure sizes in generic dark energy models

On the stability of cubic galileon accretion

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