Abstract
We performed N-body simulation on special-purpose computer, GRAPE-4, to investigate the structure of dark matter halos. Universal profile proposed by Navarro, Frenk, and White (1996), which has cusp with density profiles ρ ∝ r −1 in density profile, cannot be reproduced in the standard Cold Dark Matter (CDM) picture of hierarchical clustering. Previous claims to the contrary were based on simulations with relatively few particles, and substantial softening. We present simulations with particle numbers an order of magnitude higher (N = 786,400), and essentially no softening, and show that typical central density profiles are clearly steeper than ρ ∝ r −1
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Fukushige, T., Marino, J. (1999). N-Body Simulation of Dark Matter Halo Formation Using Grape. In: Miyama, S.M., Tomisaka, K., Hanawa, T. (eds) Numerical Astrophysics. Astrophysics and Space Science Library, vol 240. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4780-4_4
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DOI: https://doi.org/10.1007/978-94-011-4780-4_4
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