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We conduct numerical experiments by evolving gaseous/stellar disks embeddedin live dark matter halos aiming at quantifying the effect of gas spatialresolution and gas content on the bar evolution. Model sequences have beenconstructed using different resolution, and gas fraction has been varied alongeach sequence within fgas=0%-50%, keeping the disk and halo propertiesunchanged. We find that the spatial resolution becomes important with anincrease in `fgas'. For the higher resolution model sequences, we observe abimodal behavior in the bar evolution with respect to the gas fraction,especially during the secular phase of this evolution. The switch from thegas-poor to gas-rich behavior is abrupt and depends on the resolution used. Thediverging evolution has been observed in nearly all basic parameterscharacterizing bars, such as the bar strength, central mass concentration,vertical buckling amplitude, size, etc. We find that the presence of the gascomponent severely limits the bar growth and affects its pattern speedevolution. Gas-poor models display rapidly decelerating bars, while gas-richmodels exhibit bars with constant or even slowly accelerating tumbling. Thegas-rich models have bar corotation (CR) radii within the disk at all times, inconstrast with gas-poor and purely stellar disks. The CR-to-bar size ratio isless than 2 for gas rich-models. We have confirmed that the disk angularmomentum within the CR remains unchanged in the gas-poor models, as long as theCR stays within the disk, but experiences a sharp drop before leveling off inthe gas-rich models. Finally, we discuss a number of observed correlationsbetween various parameters of simulated bars, e.g., bar sizes and gasfractions, bar strength and buckling amplitude, bar strength and its size, etc.

Dark Matter Halos and Evolution of Bars in Disk Galaxies: Varying Gas Fraction and Gas Spatial Resolution