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Short (inner) bars of sub-kiloparsec radius have been hypothesized to be animportant mechanism for driving gas inflows to small scales, thus feedingcentral black holes. Recent numerical simulations have shown that the growth ofcentral black holes in galaxies can destroy short bars, when the black holereaches a mass of $\sim 0.1\%$ of the total stellar mass of the galaxy. Westudy $N$-body simulations of galaxies with single and double bars to track thelong-term evolution of the central stellar mass distribution. We find that thedestruction of the short bar contributes significantly to the growth of thebulge. The final bulge mass is roughly equal to the sum of the masses of theinitial pseudo bulge and short bar. The initially boxy/peanut-shaped bulge ofS\'ersic index $n\lesssim1$ is transformed into a more massive, compactstructure that bears many similarities to a classical bulge, in terms of itsmorphology ($n \approx 2$), kinematics (dispersion-dominated, isotropic), andlocation on standard scaling relations (Kormendy relation, mass-size relation,and correlations between black hole mass and bulge stellar mass and velocitydispersion). Our proposed channel for forming classical bulges relies solely onthe destruction of short bars without any reliance on mergers. We suggest thatsome of the less massive, less compact classical bulges were formed in thismanner.

A New Channel of Bulge Formation via The Destruction of Short Bars