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The evolution of disk galaxies in modified gravity is studied by usinghigh-resolution N-body simulations. More specifically, we use the weak fieldlimit of two modified gravity theories, i.e., nonlocal gravity (NLG) andscalar-tensor-vector gravity known as MOG, and ignore the existence of darkmatter halo. On the other hand, we construct the same models in the standarddark matter model and compare their dynamics with the galactic models inmodified gravity. It turns out that there are serious differences betweengalactic models in these different viewpoints. For example, we explicitly showthat the galactic models in modified gravity, host faster bars compared to thedark matter case. On the other hand, final stellar bars are weaker in modifiedgravity. These facts are not new and have already been reported in our previoussimulations for exponential galactic models. Therefore, our main purpose inthis study is to show that the above-mentioned differences, with emphasis onthe speed of the bars, are independent of the initial density profile of theadopted disk/halo. To do so, we employ different profiles for the disk and haloand show that the results remain qualitatively independent of the initialgalactic models. Moreover, a more accurate method has been used to quantify thekinematic properties of the stellar bar. Our results imply that contrary to thedark matter models, bars in modified gravity are fast rotators which neverleave the fast-bar region until the end of the simulation.

Does modified gravity predict fast stellar bars in spiral galaxies?