Angular Diameter Distances in Clumpy Friedmann Universes : Astrophysics and Relativity
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概要
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Solving null-geodesic equations, behavior of angular diameter distances is studied in inhomogeneous cosmological models, which are given by performing N-body simulations with the CDM spectrum. The distances depend on the separation angle θ of ray pairs, the mass m and the radius r_s of particles consisting of galaxies and dark matter balls, and cosmological model parameters. The calculated distances are compared with the Dyer-Roeder angular diameter distance with the clumpiness parameter α (=0-1), and for each ray pair the corresponding α is determined. Shooting many ray pairs, we derive statistical quantities such as the average value (α^^-), the dispersion (σ_α), and the distribution of α. It is found in four cosmological models with (Ω_0,λ_0)=(1,0), (0.2,0), (0.4,0), (0.2,0.8) for the particle parameters m ≃ 2×10^<12> M_≃ and r_s=(10-40)h^<-1> kpc that (1) α^^- is nearly equal to 1 or the Friedmann distance is best fitted, (2) σ_α decreases with the increase of the redshift z and radius r_s, (3) for θ ≫ 1 arcsec, σ_α is very small, but for θ < 1 arcsec it is so large that the use of only the the Friedmann distance (α=1) may cause some errors for quantitative analysis of cosmological lensing, (4) the distribution of α is symmetric and asymmetric for σ_α< 0.5 and > 0.8, respectively, and (5) σ_α is smallest and largest in models with (1,0) and (0.2,0), respectively. The cosmological constant has the role of decreasing σ_α.
- 理論物理学刊行会の論文
- 1998-07-25
著者
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Tomita K
Tokyo Development Center Yaskawa Electric Mfg.co. Ltd
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Tomita K
Yukawa Institute For Theoretical Physics Kyoto University
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Tomita Kenji
Yukawa Institute For Theoretical Physics Kyoto University
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