Dark halos formed via dissipationless collapse: 1. shapes and alignment of angular momentum

Aug 19, 1992
56 pages
Published in:
  • Astrophys.J. 399 (1992) 405
Report number:
  • LA-UR-91-4071

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Abstract: (ADS)
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.
Note:
  • Fermilab Library Only
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