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Inner Structure of Dark Matter Halos

Published online by Cambridge University Press:  26 May 2016

Toshiyuki Fukushige ,
Atsushi Kawai  and
Junichiro Makino
Toshiyuki Fukushige
Affiliation:
Department of General Systems Studies, College of Arts and Science, University of Tokyo, 3-8-1 Komaba, Meguro, Tokyo, Japan
Atsushi Kawai
Affiliation:
Faculty of Human and Social Studies, Saitama Institute of Technology, 1690 Fusaiji, Okabe, Ohsato, Saitama, Japan
Junichiro Makino
Affiliation:
Department of Astronomy, School of Sciences, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, Japan

Abstract

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We investigate the structure of the dark matter halo formed in the cold dark matter scenarios by N-body simulations with parallel treecode on GRAPE cluster systems (Fukushige, Kawai, Makino 2003). We simulated 8 halos with the mass of 4.4 × 1014M⊙ to 1.6 × 1015M⊙ in the SCDM and LCDM model using up to 30 million particles. With the resolution of our simulations, the density profile is reliable down to 0.2 percent of the virial radius. Our results show that the slope of inner cusp within 1 percent virial radius is shallower than −1.5, and the radius where the shallowing starts exhibits run-to-run variation, which means the innermost profile is not universal.

Type
Part 3: Central Density Cusps, Thin Disks, and Dark Halo Substructure
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 99 - 100
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

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