Bars in Cuspy Dark Halos

Bars in Cuspy Dark Halos

To be published in the proceedings of IAU Symposium 254: The Galaxy Disk in Cosmological Context
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Here are links to the Quicktime animations referenced in the article.

Animation 1 shows the evolution of the disks in six models with increasing resolution in and either lose the bar or suffer from heating affects. At higher resolution, the behaviour is similar exhibiting the buckling instability and relaxation to a bar in quasi-equilibrium that gradually lengthens and slows down.

Animation 2 shows the multi-mass model with Nh = 10^8 in an inertial frame and illustrates how the bar grows from noise from the inside out saturating as a thin bar on reaching the corotation radius and then evolving into a fatter bar with a peanut-shaped bulge after the buckling instability.

Animation 3 shows the bar instability in the co-rotating frame from a long view and a close-up of the centre.

Animation 4 presents the time evolution of the differential number density in phase space and reveals how the resonances move through a large fraction of the halo mass as the bar evolves.

Animation 1 shows the evolution of the disks in six models with increasing resolution in and either lose the bar or suffer from heating affects. At higher resolution, the behaviour is similar exhibiting the buckling instability and relaxation to a bar in quasi-equilibrium that gradually lengthens and slows down.	Animation 2 shows the multi-mass model with Nh = 10^8 in an inertial frame and illustrates how the bar grows from noise from the inside out saturating as a thin bar on reaching the corotation radius and then evolving into a fatter bar with a peanut-shaped bulge after the buckling instability.
Animation 3 shows the bar instability in the co-rotating frame from a long view and a close-up of the centre.	Animation 4 presents the time evolution of the differential number density in phase space and reveals how the resonances move through a large fraction of the halo mass as the bar evolves.