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The characteristics of the galactic bars that are prone to suffer a damagingimpact from a massive central black hole are examined using flat stellar disks.We construct three disk model groups that consist of exponential disks with onetype of velocity distribution and Kuzmin-Toomre disks with two different typesof exact equilibrium distribution function. For each disk model group, threedisks that have different typical Toomre's Q values are evolved to form barsthrough dynamical instability. Once a bar is fully developed, a black hole(BH), whose mass is 1% of the disk mass, is adiabatically added at the centerof the disk. Our results show that lower-amplitude bars, that is, weaker barsare dissolved more easily by that BH. We have found that this destructibilityis rooted in the characteristic feature that the bar formed spontaneouslybecomes shorter in length and rounder in shape with decreasing bar amplitude.Since such weaker bars are found to originate from colder disks in each diskmodel group, it follows that for a given form of velocity structure, thecoldness of an initial disk determines whether the bar produced in that disk isfavorable to dissolution induced by a massive central BH. In addition, theexistence of bar-dissolved galaxies of the kind studied here is also discussed.

Destructible Bars in Disk Galaxies under the Dynamical Influence of a Massive Central Black Hole