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Bars and the connection between dark and visible matter

Published online by Cambridge University Press:  26 May 2016

E. Athanassoula
E. Athanassoula*
Affiliation:
Observatoire, 2 place Le Verrier, 13248 Marseille cedex 04, France

Abstract

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Isolated barred galaxies evolve by redistributing their internal angular momentum, which is emitted mainly at the inner disc resonances and absorbed mainly at the resonances in the outer disc and the halo. This causes the bar to grow stronger and its pattern speed to decrease with time. A massive, responsive halo enhances this process. I show correlations and trends between the angular momentum absorbed by the halo and the bar strength, pattern speed and morphology. It is thus possible to explain why some disc galaxies are strongly barred, while others have no bar, or only a short bar or an oval. in some cases, a bar is found also in the halo component. This “halo bar” is triaxial, but more prolate-like, is shorter than the disc bar and rotates with roughly the same pattern speed. I finally discuss whether bars can modify the density cusps found in cosmological CDM simulations of dark matter haloes.

Type
Part 8: Bars
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 255 - 264
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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