  The dark matter halo properties, for example, mass, spin and concentration
play a significant role in the formation and evolution of bars in disk
galaxies. This study highlights the importance of a new parameter: the dark
matter halo angular momentum distribution in the central region of disk. We
experiment with N-body galaxy models having a disk and dark matter similar to
Milky Way-type galaxies. In these models, we vary the discontinuity of the
angular momentum distribution of the halo (the total spin is the same for all
models). Our N-body experiments suggest that bar forms in all models after a
few Gyr of disk evolution. However, in the secular evolution of the bar, as we
evolve these models until 9.78 Gyr, the bar gains its strength in the model
with the most continuous halo angular momentum distribution, and the bar loses
strength for the most discontinuous halo angular momentum distribution. The
secular evolution of the bar suggests that box/peanut/x-shaped bulges similar
to those found in the Milky Way disk should be more pronounced in halos with
continuous halo angular momentum distributions. This study demonstrates the
importance of the initial condition setup of galaxy systems, namely the
discontinuity in the dark matter halo angular momentum distribution for a given
density distribution, on the bar secular evolution in the disk galaxy
simulations. Further, this study helps reconcile the conflicting results of bar
secular evolution in a high-spinning halo of the recent literature.
