منابع مشابه
Distribution Function in Center of Dark Matter Halo
N-body simulations of dark matter halos show that the density profiles of halos behave as ρ(r) ∝ r−α(r), where the density logarithmic slope α ≃ 1 ∼ 1.5 in the center and α ≃ 3 ∼ 4 in the outer parts of halos. However, some observations are not in agreement with simulations in the very central region of halos. The simulations also show that velocity dispersion anisotropy parameter β ≈ 0 in the ...
متن کاملDistribution Function of Dark Matter with Constant Anisotropy
N-body simulations of dark matter halos show that the density is cusped near the center of the halo. The density profile behaves as r in the inner parts, where γ ≃ 1 for the NFW model and γ ≃ 1.5 for the Moore’s model, but in the outer parts, both models agree with each other in the asymptotic behavior of the density profile. The simulations also show the information about anisotropy parameter ...
متن کاملCoarse-graining the distribution function of cold dark matter II
We study analytically the coarse and fine-grained distribution function established by the self-similar infall of collisionless matter. We find this function explicitly for isotropic and spherically symmetric systems in terms of cosmological initial conditions. The coarse-grained function is structureless and steady but the familiar phase space sheet sub-structure is recovered in the fine-grain...
متن کاملDark matter distribution function from non-extensive statistical mechanics
We present an analytical and numerical study of the velocity distribution function of self gravitating collisionless particles, which include dark matter and star clusters. We show that the velocity distribution derived through the Eddington’s formula is identical to the analytical one derived directly from the generalized entropy of non-extensive statistical mechanics. This implies that self g...
متن کاملThe Distribution of Dark Matter in Spirals
In the past years a wealth of observations allowed to unravel the structural properties of the Dark Matter Halos around spirals. First, their rotation curves follow an Universal profile (URC) that can be described in terms of an exponential thin stellar disk and a dark halo with a constant density core, whose relative importance increases with galaxy luminosity. Careful studies of individual ob...
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2006
ISSN: 1550-7998,1550-2368
DOI: 10.1103/physrevd.73.023524