Dissipationless galaxy formation from non-isolated density perturbations

Details Dissipationless galaxy formation from non-isolated density perturbations Dissipationless galaxy formation from non-isolated density perturbations

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...249....5v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 249, no. 1, Sept. 1991, p. 5-13.

Astronomy and Astrophysics

Astrophysics

13

Galactic Evolution, Galactic Nuclei, Particle Energy, Perturbation Theory, Density Distribution, Energy Dissipation, Energy Distribution, Universe

Scientific paper

The n-body code is developed to investigate the evolution of protogalactic bound objects by considering the dynamical effects of the neighboring material and the extensive mass environment. The final radial profile of the density perturbation differs from that of the similarity solution since the binding energies between the particles are redistributed and because the initial profile is aspherical. The model generates a system of a rotating bar embedded in a triaxial rotating halo similar to that of the similarity solution, but the differences suggest significant variations in final radius and binding energies.

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