N-body equilibrium figures of early-type galaxies. I - Global structures

Statistics – Computation

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Elliptical Galaxies, Galactic Evolution, Galactic Structure, Gravitational Collapse, Many Body Problem, Anisotropy, Computational Astrophysics, Density Distribution, Energy Distribution, Galactic Rotation, Systems Stability

Scientific paper

The equilibrium structure of early-type galaxies is investigated using an N-body numerical simulation. Rotation, cold initial conditions, and anisotropy seem essential to obtain flattened final configurations modeling elliptical galaxies. It is shown that small values of the anisotropy parameter lead to triaxial end-products even if the initial conditions are not very cold. Particular systems can be constructed by properly choosing values for the initial parameters. The obtained kinematic profiles are compatible with those of elliptical galaxies, but significant deviations from ellipticity occur. In particular, box and peanut shapes are produced by a 'natural' self-gravitating evolution from cold initial conditions. The final density profiles follow de Vaucouleurs R exp 1/4 laws. The energy distributions per unit mass are compatible with a power law with exponent -5/2 for large ones, as predicted by the statistical mechanics of violent relaxation and a Keplerian potential in the outer regions.

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