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Dark halos formed via dissipationless collapse. I - Shapes and alignment of angular momentum
Warren, Michael S.; Quinn, Peter J.; Salmon, John K.; Zurek, Wojciech H.
AA(Los Alamos National Lab., NM), AB(Mount Stromlo and Siding Spring Observatoires, Canberra, Australia), AC(California Inst. of Technology, Pasadena), AD(Los Alamos National Laboratory, NM)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 2, p. 405-425. (ApJ Homepage)
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NASA/STI Keywords:
Angular Momentum, Dark Matter, Gravitational Collapse, Many Body Problem, Computational Astrophysics, Halos
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We use N-body simulations on highly parallel supercomputers to study the structure of Galactic dark matter halos. The systems form by gravitational collapse from scale-free and more general Gaussian initial density perturbations in an expanding 400 Mpc-cubed spherical slice of an Einstein-deSitter universe. We analyze the structure and kinematics of about 100 of the largest relaxed halos in each of 10 separate simulations. A typical halo is a triaxial spheroid which tends to be more often prolate than oblate. These shapes are maintained by anisotropic velocity dispersion rather than by angular momentum. Nevertheless, there is a significant tendency for the total angular momentum vector to be aligned with the minor axis of the density distribution.

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Database: Astronomy
arXiv e-prints