SearcharxivSearch

arXiv · astro-ph/9810190

N-point correlations in CDM and $Ω$CDM Simulations

Abstract

Higher order statistics are investigated in ($Ω$)CDM universes by analyzing $500\mpc$ high resolution tree N-body simulations with both $Ω= 1$, and $Ω< 1$. The amplitudes of the N-point correlation functions are calculated from moments of counts-in-cells determined by a pair of new algorithms especially developed for large simulations. This approach enables massive oversampling with $\simeq 10^{9-14}$ cells for accurate determination of factorial moments from up to 47 million particles in the scale range of $8 \kpc - 125\mpc$. Thorough investigation shows that there are three scale ranges in the simulations: $\ge 8\mpc$, weakly non-linear regime, where perturbation theory applies with utmost precision, $1\mpc - 8\mpc$, the non-linear plateau, and finally $\le 1\mpc$, a regime where dynamical discreteness effects dominate the higher order statistics. In the physically relevant range of $1\mpc-125\mpc$ the results i) confirm the validity of perturbation theory in the weakly non-linear regime, ii) establish the existence of a plateau in the highly non-linear regime similar to the one observed in scale free simulations iii) show extended perturbation theory to be an excellent approximation for the non-linear regime iv) find the time dependence of the $S_N$'s to be negligible in both regimes v) in comparison with similar measurements in the EDSGC survey, strongly support $Ω< 1$ with no biasing vi) show that the formulae of Szapudi & Colombi (1996) provide a good approximation for errors on higher order statistics measured in N-body simulations.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Istvan Szapudi, Thomas Quinn, Joachim Stadel, George Lake. 1998-10-13. N-point correlations in CDM and $Ω$CDM Simulations. https://doi.org/10.1086/307192

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Scaling of Black Hole Accretion Discs from Gamma-Ray Bursts and Black Hole X-Ray Binaries to Active Galactic Nuclei

I consider how physical processes scale over eight orders of magnitude in black hole mass, from stellar masses in gamma-ray bursts (GRB) and black-hole X-ray binaries (BHXRB) to supermassive active galactic nuclei (AGN). Accretion rates onto stellar mass black holes range over more than sixteen orders of magnitude, from the lower luminosity BHXRB to GRB. These enormous parameter ranges correspond to qualitative as well as quantitative differences in behavior. The fundamental questions involve the balance between nonequilibrium and thermalized plasmas. When energy fluxes exceed a critical value $\sim 10^{29}$ erg/cm$^2$s, as in GRB, a black-body equilibrium pair plasma forms. At the lower fluxes found in AGN, BHXRB and microquasars, accretion power electrodynamically accelerates a small number of very energetic particles, explaining their non-thermal spectra and the high energy gamma-ray emission of blazars. Ultra-high energy cosmic rays may be accelerated by massive black holes, otherwise undetectable, with very low thermal luminosities. New-born fast high-field pulsars may be in the black-body equilibrium regime, resembling SGR in permanent outburst. I also consider the question, significant for the acceleration of nonthermal particles in GRB outflows, of whether collisionless plasmas interpenetrate rather than forming hydrodynamic shocks, and propose this as an alternative to internal shock models of GRB. A new appendix attempts to explain why AGN are, proportionally, more efficient accelerators of energetic particles than stellar mass black holes.

astro-ph

Two 3-Branes in Randall-Sundrum Setup and Current Acceleration of the Universe

Five-dimensional spacetimes of two orbifold 3-branes are studied, by assuming that {\em the two 3-branes are spatially homogeneous, isotropic, and independent of time}, following the so-called "bulk-based" approach. The most general form of the metric is obtained, and the corresponding field equations are divided into three groups, one is valid on each of the two 3-branes, and the third is valid in the bulk. The Einstein tensor on the 3-branes is expressed in terms of the discontinuities of the first-order derivatives of the metric coefficients. Thus, once the metric is known in the bulk, the distribution of the Einstein tensor on the two 3-branes is uniquely determined. As applications, we consider two different cases, one is in which the bulk is locally $AdS_{5}$, and the other is where it is vacuum. In some cases, it is shown that the universe is first decelerating and then accelerating. The global structure of the bulk as well as the 3-branes is also studied, and found that in some cases the solutions may represent the collision of two orbifold 3-branes. The applications of the formulas to the studies of the cyclic universe and the cosmological constant problem are also pointed out.

astro-ph

A Revolution in Science: the Eclipse Expeditions of 1919

The first direct experimental test of Einstein's theory of general relativity involved a pair of expeditions to measure the bending of light at a total solar eclipse that took place one hundred years ago, on 29 May 1919. So famous is this experiment, and so dramatic was the impact on Einstein himself, that history tends not to recognise the controversy that surrounded the results at the time. In this article, I discuss the experiment in its scientific and historical background context and explain why it was, and is, such an important episode in the development of modern physics.

astro-ph