作者: Emilio Romano-Díaz , Yehuda Hoffman , Clayton Heller , Isaac Shlosman
DOI: 10.1086/592687
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摘要: We study the central dark matter (DM) cusp evolution in cosmologically grown galactic halos. Numerical models with and without baryons (baryons+DM, hereafter BDM model, pure DM, PDM respectively) are advanced from identical initial conditions, obtained using Constrained Realization method. The DM properties contrasted by a direct comparison of baryonic models. find divergent between within inner few × 10 kpc region. model forms an R−1 as expected, while larger isothermal R−2 instead. is stable until z ~ 1 when it gradually levels off. This leveling proceeds inside out final density slope shallower than –1 3 (i.e., expected size cusp), tending to flat core ~2 kpc. effect cannot be explained finite resolution our code which produces only 5% difference gravitationally softened force exact Newtonian point masses at center. Neither related energy feedback stellar or angular momentum transfer bar. Instead can associated action DM+baryon subhalos heating up region via dynamical friction forcing flow "cool" down. process described here not limited low efficient intermediate even high z.