The large-scale structure of the universe: Turbulence, intermittency, structures in a self-gravitating medium

Shandarin, Sergei F.; Zel’dovich, Ya. B.

doi:10.1103/revmodphys.61.185

Cited by 868 publications

(738 citation statements)

References 134 publications

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“…In this paper we construct sufficient integral criteria for breaking within the model (3), (4) and verify what the functional conditions of the theorem [1] correspond to those for the given system. Our main conjecture is the following: breaking in the 3D case within the system yields a violation of Sobolev space already for q = 2 instead of q ≥ 3 in the theorem [1].…”

Section: Introductionmentioning

confidence: 99%

“…According to the pioneering idea of Ya.B. Zeldovich [3], the formation of proto-galaxies due to breaking of stellar dust can be described by the system (3), (4) (see also the review [4]). It should be noticed also that recently [5,6] the mechanism of breaking was used to explain collapse in incompressible fluids when, instead of the breaking of fluid particles, the breaking of vortex lines can happen which results in a blow-up of vorticity.…”

Section: Introductionmentioning

confidence: 99%

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Towards a sufficient criterion for collapse in 3D Euler equations

Кузнецов¹

2003

Physica D: Nonlinear Phenomena

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Towards a sufficient criterion for collapse in 3D Euler equations

Кузнецов¹

2003

Physica D: Nonlinear Phenomena

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“…It is worth noting that in Eq. (20), the density fluctuation is given in a formally exact form, even though we keep only the linear term in this paper. The peculiar velocity appearing in Eqs.…”

Section: Perturbationmentioning

confidence: 99%

“…This description provides relatively accurate values even in a quasi-linear regime in the structure formation scenario [12,17,18,19,20,21,22,23,24,25,26,27,28]. (Especially, for the case of the dust fluid, this approximation is called the Zel'dovich approximation (ZA)).…”

mentioning

confidence: 99%

Non-Gaussianity of the density distribution in accelerating universes

Tatekawa

Mizuno

2006

J. Cosmol. Astropart. Phys.

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Abstract. According to recent observations, the existence of the dark energy has been considered. Even though we have obtained the constraint of the equation of the state for dark energy (p = wρ) as −1 ≤ w ≤ −0.78 by combining WMAP data with other astronomical data, in order to pin down w, it is necessary to use other independent observational tools. For this purpose, we consider the w dependence of the non-Gaussianity of the density distribution generated by nonlinear dynamics. To extract the non-Gaussianity, we follow a semi-analytic approach based on Lagrangian linear perturbation theory, which provides an accurate value for the quasi-nonlinear region. From our results, the difference of the non-Gaussianity between w = −1 and w = −0.5 is about 4% while that between w = −1 and w = −0.8 is about 0.9%. For the highly non-linear region, we estimate the difference by combining this perturbative approach with N-body simulation executed for our previous paper. From this, we can expect the difference to be more enhanced in the low-z region, which suggests that the non-Gaussianity of the density distribution potentially plays an important role for extracting the information of dark energy.PACS numbers: 04.25. Nx, 95.30.Lz, 98.65.Dx

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“…The work presented here is meant for large-scales and hence does not classify zones of vanishing velocities in the multi-stream regions. The fluid equation relating the velocity v i , density ρ and perturbations of the gravitational potential φ are [17,23] ,…”

Section: The Velocity and The Density Fields In The Zel'dovich Approxmentioning

confidence: 99%

Critical points of the cosmic velocity field and the uncertainties in the value of the Hubble constant

Liu¹,

Mohayaee²,

Naselsky³

2016

J. Cosmol. Astropart. Phys.

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Abstract. The existence of critical points for the peculiar velocity field is a natural feature of the correlated vector field. These points appear at the junctions of velocity domains with different orientations of their averaged velocity vectors. Since peculiar velocities are the important cause of the scatter in the Hubble expansion rate, we propose that a more precise determination of the Hubble constant can be made by restricting analysis to a subsample of observational data containing only the zones around the critical points of the peculiar velocity field, associated with voids and saddle points. On large-scales the critical points, where the first derivative of the gravitational potential vanishes, can easily be identified using the density field and classified by the behavior of the Hessian of the gravitational potential. We use high-resolution N-body simulations to show that these regions are stable in time and hence are excellent tracers of the initial conditions. Furthermore, we show that the variance of the Hubble flow can be substantially minimized by restricting observations to the subsample of such regions of vanishing velocity instead of aiming at increasing the statistics by averaging indiscriminately using the full data sets, as is the common approach.

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The large-scale structure of the universe: Turbulence, intermittency, structures in a self-gravitating medium

Cited by 868 publications

References 134 publications

Towards a sufficient criterion for collapse in 3D Euler equations

Towards a sufficient criterion for collapse in 3D Euler equations

Non-Gaussianity of the density distribution in accelerating universes

Critical points of the cosmic velocity field and the uncertainties in the value of the Hubble constant

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