Dynamical evolution driven by bars and interactions : Input from numerical simulations

Abstract

We discuss the evolution of a disc galaxy due to the formation of a bar and, subsequently, a peanut. After the formation stage there is still considerable evolution, albeit slower. In purely stellar cases the pattern speed of the bar decreases with time, while its amplitude grows. However, if a considerable gaseous component is present in the disc, the pattern speed may increase with time, while the bar strength may decrease. In some cases the gas can be brought sufficiently close to the center to create a strong central concentration, which, in turn, may modify the properties of the bar. More violent evolution can take place during interactions, so that some disc substructures can be either formed or destroyed in a time scale which is small compared to a Hubble time. These include spirals, bars, bridges, tails, rings, thick discs and bulges. In some cases interactions may lead to mergings. We briefly review comparisons of the properties of merger remnants with those of elliptical galaxies, both for the case of pairwise mergings and the case of multiple mergings.

10 pages, no figures, review paper for the Euroconference II on Evolution of Galaxies at Reunion, Kluwer academic press, eds. M. Sauvage et al

References in corpus (6)

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• When Should We Treat Galaxies as Isolated?
• Simulating non-axisymmetric flows in disc galaxies
• The role of environment on the evolution of disc galaxies density profiles New insights from simulations and comparison to Euclid data