منابع مشابه
Early structure in Λ CDM
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We use a novel technique to simulate the growth of one of the most massive progenitors of a supercluster region from redshift z ∼ 80, when its mass was about 10M⊙, until the present day. Our nested sequence of N–body resimulations allows us to study in detail the structure both of the dark matter object itself and of its environment. Our effective resolution is optimal at redshifts of 49, 29, 1...
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Coupling the dark matter (DM) and baryonic components in galaxies via dynamical friction (by allowing the latter to be clumpy) leads to energy input into the DM. The resulting expanding tendency in the DM component overcomes the competing effect of adiabatic contraction, resulting from the shrinking gas component, and leads to a nearly constant density core. The baryonic mass inflow also leads ...
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Dark-matter (DM) halos are the scaffolding around which galaxies and clusters are built. They form when the gravitational instability of primordial density fluctuations causes regions which are denser than average to slow their cosmic expansion, recollapse, and virialize. Understanding the equilibrium structure of these halos is thus a prerequisite for understanding galaxy and cluster formation...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2005
ISSN: 0035-8711,1365-2966
DOI: 10.1111/j.1365-2966.2005.09509.x