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2013MNRAS.429.1949A - Mon. Not. R. Astron. Soc., 429, 1949-1969 (2013/March-1)
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties.
ATHANASSOULA E., MACHADO R.E.G. and RODIONOV S.A.
Abstract (from CDS):
Halo triaxiality has a dual influence on bar strength. In the very early stages of the simulation it induces bar formation to start earlier. On the other hand, during the later, secular evolution phase, triaxial haloes lead to considerably less increase of the bar strength than spherical ones. The shape of the halo evolves considerably with time. We confirm previous results of gas-less simulations that find that the inner part of an initially spherical halo can become elongated and develop a halo bar. However we also show that, on the contrary, in gas-rich simulations, the inner parts of an initially triaxial halo can become rounder with time. The main body of initially triaxial haloes evolves towards sphericity, but in initially strongly triaxial cases it stops well short of becoming spherical. Part of the angular momentum absorbed by the halo generates considerable rotation of the halo particles that stay located relatively near the disc for long periods of time. Another part generates halo bulk rotation, which, contrary to that of the bar, increases with time but stays small. Thus, in our models there are two non-axisymmetric components rotating with different pattern speeds, namely the halo and the bar, so that the resulting dynamics have strong similarities to the dynamics of double bar systems.
Abstract Copyright: © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2012)
Journal keyword(s): galaxies: evolution - galaxies: haloes - galaxies: kinematics and dynamics - galaxies: structure
Simbad objects: 4
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