Evolution of galaxies along the Hubble Sequence

Details Evolution of galaxies along the Hubble Sequence Evolution of galaxies along the Hubble Sequence

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf..645b&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

Mathematics

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Scientific paper

The evolution of galaxies is governed by three major mechanisms: inner dynamics, galaxy interactions and mergers, and accretion of intergalactic gas by galaxies. Spiral galaxies can be classified as late-type (small bulge) and early-type (massive bulge) systems. Inner secular evolution makes spiral galaxies evolve towards early types, while in the same time gas accretion, predicted by cosmological simulations, make them return to late-type classes. Both phenomenon govern the evolution the bulge-to-disk mass ratio and the presence of spiral arms and bars in the disk. Minor galaxy mergers (with mass ratios larger than 10:1) only cause small disturbances to the morphology of spiral galaxies. At the opposite, major mergers (mass ratios 1:1 to 4:1) form elliptical galaxies. We have shown that intermediate mergers (10:1-4:1) form disk galaxies with elliptical-like kinematics, similar to the observed lenticular S0s. We have also shown that several successive mergers in the range of mass ratios 10:1-4:1 can form elliptical galaxies with a larger efficiency than single major mergers. The study of all these phenomenon enables us to give an overview of the various mechanisms that make galaxies evolve along the Hubble sequence.

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