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A Database of COBENormalized CDM Simulations (Abbreviated Version)
, 1999
"... This paper is an abbreviated version of our original manuscript. We wrote this abbreviated version in order to meet the size limitations imposed by the astroph archive. The original manuscript, which has been submitted to The Astrophysical Journal, can be obtained by contacting the authors. We have ..."
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have simulated the formation and evolution of largescale structure in the universe, for 68 different COBEnormalized cosmological models. For each cosmological model, we have performed between 1 and 3 simulations, for a total of 160 simulations. This constitutes the largest database of cosmological
COBE AND CLUSTERNORMALIZED CDM SIMULATIONS
, 2000
"... We introduce a set of four new publicly available Nbody simulations, the most recent additions to the Texas P 3 M Database. Our models probe the less studied parameter space region of moderate volume (100h −1 Mpc box) combined with fine mass resolution ( ∝ 10 12 M⊙, roughly comparable to a L ⋆ gala ..."
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⋆ galaxy), making these simulations especially suitable for study of major largescale structure (LSS) features such as voids, and for comparison with the largest threedimensional redshift surveys currently available. Our cosmological models (LCDM, TOCDM, OCDM, TCDM) are all COBEnormalized, and when
Largescale structure in COBEnormalized cold dark matter cosmogonies
, 1997
"... We study the clustering of the mass distribution in cold dark matter models using large cosmological Nbody simulations. We investigate spatiallyflat models with a cosmological constant and scaleinvariant (n = 1) primordial power spectra, as well as openbubble inflation models. All the models we ..."
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consider are normalized according to the fluctuation amplitude measured in the COBEDMR microwave background anisotropy data. With an age of the universe t0 ≈ 14 Gyr (12 Gyr) for the flat (open) models, a baryon mass density parameter ΩB = 0.0125h −2, and a reasonable assessment of the systematic
COBEDMRNORMALIZED OPEN CDM COSMOGONIES
, 1996
"... Cutsky orthogonal mode analyses of the COBEDMR 53 and 90 GHz sky maps are used to determine the normalization of a variety of open cosmogonical models based on the cold dark matter scenario. To constrain the allowed cosmologicalparameter range for these open cosmogonies, the predictions of the DM ..."
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Cutsky orthogonal mode analyses of the COBEDMR 53 and 90 GHz sky maps are used to determine the normalization of a variety of open cosmogonical models based on the cold dark matter scenario. To constrain the allowed cosmologicalparameter range for these open cosmogonies, the predictions
ClusterGalaxy Correlations in CDM Models
, 1997
"... We study the ability of COBEnormalized CDM models to reproduce observed properties of the distribution of galaxies and clusters using Nbody numerical simulations. We analyze the galaxygalaxy and clustergalaxy twopoint correlation functions, ξgg and ξcg, in open (Ω0 = 0.4, ΩΛ = 0, σ8 = 0.75), and ..."
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We study the ability of COBEnormalized CDM models to reproduce observed properties of the distribution of galaxies and clusters using Nbody numerical simulations. We analyze the galaxygalaxy and clustergalaxy twopoint correlation functions, ξgg and ξcg, in open (Ω0 = 0.4, ΩΛ = 0, σ8 = 0
XRAY CLUSTERS IN A CDM+Λ UNIVERSE: A DIRECT, LARGESCALE, HIGH RESOLUTION, HYDRODYNAMIC SIMULATION
, 1993
"... A new, threedimensional, shock capturing, hydrodynamic code is utilized to determine the distribution of hot gas in a CDM+Λ model universe. Periodic boundary conditions are assumed: a box with size 85h−1Mpc, having cell size 0.31h −1 Mpc, is followed in a simulation with 270 3 = 10 7.3 cells. We ad ..."
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in contrast to a slight increase in the number density for standard Ω = 1, CDM model. This COBEnormalized CDM+Λ model produces approximately the same
ReesSciama Effect in a CDM Universe
, 1995
"... The ReesSciama (RS) effect produces fluctuations in the cosmic microwave background (CMB) through the timedependent gravitational potential in the nonlinear stages of evolution. I investigate the RS effect on the CMB angular power spectrum Cl for several CDM models by combining the results of Nbo ..."
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body simulations with second order perturbation theory. The amplitude of the RS fluctuations peaks at l ∼ 100 − 300, where it gives ∆T/T ∼ 10 −7 − 10 −6 for a wide range of models. This is at least an order of magnitude below the COBE normalized primary contribution. RS fluctuations could be a dominant source
XRay Clusters From A High Resolution Hydrodynamic Ppm Simulation Of The Cdm Universe
, 1994
"... A new three dimensional Piecewise Parabolic Method (PPM) based hydrodynamic code is utilized to compute the distribution of hot gas in the standard COBE normalized CDM universe. Utilizing periodic boundary conditions, a box with size 85h 01 Mpc having cell size 0:31h 01 Mpc, is followed in a sim ..."
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A new three dimensional Piecewise Parabolic Method (PPM) based hydrodynamic code is utilized to compute the distribution of hot gas in the standard COBE normalized CDM universe. Utilizing periodic boundary conditions, a box with size 85h 01 Mpc having cell size 0:31h 01 Mpc, is followed in a
THE LYMAN ALPHA FOREST FROM GRAVITATIONAL COLLAPSE IN THE CDM+Λ MODEL
, 1995
"... We use an Eulerian hydrodynamic cosmological simulation to model the Lyα forest in a spatially flat, COBE normalized, cold dark matter model with Ω = 0.4, and find that the intergalactic, photoionized gas is predicted to collapse into sheetlike and filamentary structures which give rise to absorpti ..."
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We use an Eulerian hydrodynamic cosmological simulation to model the Lyα forest in a spatially flat, COBE normalized, cold dark matter model with Ω = 0.4, and find that the intergalactic, photoionized gas is predicted to collapse into sheetlike and filamentary structures which give rise
Two body relaxation in CDM simulations
, 2008
"... A standard technique to study the formation and evolution of gravitating systems is to perform an Nbody simulation in which the mass distribution is discretised into a series of softened point particles. This solution can be exact for a ..."
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A standard technique to study the formation and evolution of gravitating systems is to perform an Nbody simulation in which the mass distribution is discretised into a series of softened point particles. This solution can be exact for a
Results 1  10
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639