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We report idealized simulations that mimic the growth of galaxy disksembedded in responsive halos and bulges. The disks manifested an almostoverwhelming tendency to form strong bars that we found very difficult toprevent. We found that fresh bars formed in growing disks after we haddestroyed the original, indicating that bar formation also afflicts continuedgalaxy evolution, and not just the early stages of disk formation. Thisbehavior raises still more insistently the previously unsolved question of howsome galaxies avoid bars. Since our simulations included only collisionlessstar and halo particles, our findings may apply to gas-poor galaxies only;however the conundrum persists for the substantial unbarred fraction of thosegalaxies. Our original objective was to study how internal dynamics rearrangedthe distribution of mass in the disk as a generalization of our earlier studywith rigid spherical components. With difficulty, we were able to constructsome models that were not strongly influenced by bars, and found that halocompression, and angular momentum exchange with the disk did not alter ourearlier conclusion that spiral activity is largely responsible for creatingsmooth density profiles and rotation curves.

Mass Distribution and Bar Formation in Growing Disk Galaxy Models