Chemo-dynamical evolution of massive spherical galaxies

Details Chemo-dynamical evolution of massive spherical galaxies Chemo-dynamical evolution of massive spherical galaxies

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...265..465t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 265, no. 2, p. 465-477.

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91

Astronomical Models, Dynamic Models, Elliptical Galaxies, Galactic Evolution, Computational Astrophysics, Galactic Mass, Metallicity, Star Formation, Stellar Evolution

Scientific paper

The evolution of massive spherical galaxies is calculated by a multicomponent hydrodynamical approach taking a detailed description of interactions into account. The final state of model galaxies with 10 exp 12 solar masses is independent of their initial density: after a collapse phase with a high solar-forming activity in the first billion yrs the model galaxies show a slow dynamical evolution resulting in an almost gas-free system with a hot galactic halo, a de-Vaucouleurs stellar surface density profile, and a distinct stellar metallicity gradient. Models with 10 exp 11 solar masses evolve similar to the 10 exp 12 solar masses galaxies, but with a less pronounced gaseous halo. Their evolution is independent of their initial density except for a different timescale due to the density dependence of the dynamical timescale.

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