Powered by Indico
Various studies have shown that dark matter halo properties like concentration, triaxiality, spin, etc., play an important role in the dynamical processes of bar instability. We have investigated the role of inner (within disk region) halo angular momentum distribution on the bar formation and evolution processes. We have performed a series of high-resolution N-body experiments with Milky Way-type disk galaxies. These models are initiated with similar disks while increasing the inner halo angular momentum of the surrounding dark matter halo. The bar triggers earlier for the model with a higher inner halo angular momentum than the lower ones, similar to studies claiming the role of halo spins. However, the bar secular evolution shows growth for all the models, irrespective of inner halo angular momentum, contradicting the role of high spin in bar secular dampening claimed in earlier studies. The model with the highest inner angular momentum shows pronounced box/peanut/x-shaped bulges compared to the lowest one. Our results on the role of halo angular momentum discontinuity show that the secular growth of the bar follows the models with continuity of the halo angular momentum. In contrast, the bar dampens in secular evolution for discontinuous angular momentum halo models. These studies provide insight into complex bar formation processes. Finally, using multiple approaches like linear perturbation theory, test particle simulation and N-body simulations, we show that dynamical friction due to dark matter on bars reduces with net prograde rotation of dark matter halos.
Colloquium Committee