Constrained Violent Relaxation to a Spherical Halo

Details Constrained Violent Relaxation to a Spherical Halo Constrained Violent Relaxation to a Spherical Halo

1999-06-08

arxiv.org/abs/astro-ph/9906133v1

Astronomy and Astrophysics

Astrophysics

25 pages, 12 figures; scheduled to appear in ApJ, vol 524, #2 (oct. 99). Figures in gif format. Preprints are also available o

Scientific paper

10.1086/307831

Violent relaxation during the collapse of a galaxy halo is known to be incomplete in realistic cases such as cosmological infall or mergers. We adopt a physical picture of strong but short lived interactions between potential fluctuations and particle orbits, using the broad framework outlined by Tremaine (1987) for incorporating incompleteness of the relaxation. We are guided by results from plasma physics, viz. the quasilinear theory of Landau damping, but allow for significant differences in our case. Crucially, wave particle scattering does not drive the system to an equilibrium distribution function of the exponential type, even in regions of phase space allowed by the constraints. The physical process is mixing without friction in ``action'' space, for which the simplest possible model is a constant phase space density modulated by the constraints. Our distribution function does not use the exponential functions of the energy prevalent in other work, which we regard as inappropriate to collisionless systems. The halo of the self-consistent, parameter-free solutions show an r^(-4) behavior in density at large r, an r^(1/4) surface brightness profile in the region 0.1-8 r_e, and a radially anisotropic velocity dispersion profile outside an isotropic core. The energy distribution seen in simulations N(E) singles out the pericenter cutoff model as the most realistic among the variants we have explored.

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