Anisotropic hubble expansion of large scale structures

Fliche, H. H.; Souriau, Jean-Marie; Triay, R.

doi:10.1007/s10714-006-0233-1

Cited by 10 publications

(8 citation statements)

References 15 publications

(17 reference statements)

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“…These notations are preferred to the usual Ω Λ = λ • and Ω K = −k • for avoiding ambiguities on the interpretation of cosmological parameters, see e.g., [8], [10]. A dimensional analysis of Eq.…”

Section: Newton-friedmann and Vacuum Modelsmentioning

confidence: 99%

Λ effect in the cosmological expansion of void

Fliche¹,

Triay²

2010

J. Cosmol. Astropart. Phys.

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We investigate the dynamical effect of the cosmological constant Λ on a single spherical vacuum void evolving in the universe within a global solution of Newton-Friedmann models. As a result, the main characteristic is that the void expands with a huge initial burst up to match asymptotically the Hubble flow. The size of voids increases with Ω • and with Λ, which is interpreted as respectively by the gravitational attraction of borders from outside regions and by the gravitational repulsion of vacuum from the inner region. The Λ-effect on the kinematics intervenes significantly by amplifying the expansion rate at redshift z ∼ 1.7 for a background density parameter Ω • ∼ 0.3. For a class of parameters values, which corresponds in GR to spatially closed Friedmann models, it is interesting to note that a test particle in the inner region moves toward the border. Such a peculiar feature shows that the empty regions are swept out ; which stands as a stability criterion. -Marseille II et du Sud Toulon-Var. Laboratoire affiliéà la FRUMAM (FR 2291).

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Section: Newton-friedmann and Vacuum Modelsmentioning

confidence: 99%

Λ effect in the cosmological expansion of void

Fliche¹,

Triay²

2010

J. Cosmol. Astropart. Phys.

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“…Thirdly, it would be interesting to search exact solutions of the non linear gravitation field equations, at least with additional symmetries, for instance spherical. Finally, we thinks this kind of approach could be useful for the Cosmology, for instance modelling the distribution of galaxies at local scale as done in [15].…”

Section: Potential Vector At Order Onementioning

confidence: 99%

Post-Newtonian expansion with Galilean covariance

de Saxcé

2020

Preprint

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The Galilean gravitation derives from a scalar potential and a vector one. Poisson's equation to determine the scalar potential has no the expected Galilean covariance. Moreover, there are three missing equations to determine the potential vector. Besides, we require they have the Galilean covariance. These are the issues addressed in the paper. To avoid the drawbacks of the PPN approach and the NCT, we merge them into a new framework. The key idea is to take care that every term of the c expansion of the fields are Galilean covariants or invariants. The expected equations are deduced by variation of the Hilbert-Einstein functional. The contribution of the matter to the functional is derived from Souriau's conformation tensor. We obtain a system of four non linear equations, solved by asymptotic expansion.

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“…Hereafter, we simply provides us with synthesis results, more information can be found in [17]. 8 The modified newtonian gravitation field reads g = Λ 3 − Gm r 3 r 9 These notations are preferred to the usual Ω Λ = λ • and Ω K = −k • for avoiding ambiguities on the interpretation of cosmological parameters, see e.g., [13], [14]. 10 Because the mapping t → a(t) = 1/(1 + z) is a monotonic function in the present investigation, their evolution with cosmic time t or with redshift z can be straightforwardly derived.…”

Section: Qualitative Analysismentioning

confidence: 99%

“…Since Hubble expansion is all the more important towards the past, the earlier the formation date the weaker this effect, according to eq. (87) 14. At first glance, on might argue that the related scale should be larger than the size of background structures in order to make the uniform density hypothesis an acceptable approximation, what looks like a dilemma.…”

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confidence: 99%

Euler-Poisson-Newton approach in Cosmology

Triay¹,

Fliche²

2007

AIP Conference Proceedings

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This lecture provides us with Newtonian approaches for the interpretation of two puzzling cosmological observations that are still discussed subject : a bulk flow and a foam like structure in the distribution of galaxies. For the first one, we model the motions describing all planar distortions from Hubble flow, in addition of two classes of planar-axial distortions with or without rotation, when spatial distribution of gravitational sources is homogenous. This provides us with an alternative to models which assume the presence of gravitational structures similar to Great Attractor as origin of a bulk flow. For the second one, the model accounts for an isotropic universe constituted by a spherical void surrounded by a uniform distribution of dust. It does not correspond to the usual embedding of a void solution into a cosmological background solution, but to a global solution of fluid mechanics. The general behavior of the void expansion shows a huge initial burst, which freezes asymptotically up to match Hubble expansion. While the corrective factor to Hubble law on the shell depends weakly on cosmological constant at early stages, it enables us to disentangle significantly cosmological models around redshift z ~ 1.7. The magnification of spherical voids increases with the density parameter and with the cosmological constant. An interesting feature is that for spatially closed Friedmann models, the empty regions are swept out, what provides us with a stability criterion.Comment: 15 pages, 1 figur

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Anisotropic hubble expansion of large scale structures

Cited by 10 publications

References 15 publications

Λ effect in the cosmological expansion of void

Λ effect in the cosmological expansion of void

Post-Newtonian expansion with Galilean covariance

Euler-Poisson-Newton approach in Cosmology

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