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We confirm that a high rate of shear at the center is able to stabilize an entire stellar disk against bar-forming (m=2) modes, irrespective of the dark halo density. Our simulations of unstable power-law disks also yield the growth rate and pattern speed of the dominant lop-sided (m=1) mode in close agreement with that predicted by linear theory in our cleanest case. The one-armed modes, which dominate models with extensive disks, can be controlled by tapering the outer disk. Two-armeddoi:10.1086/318228 fatcat:ujzscbd6dzfnfbi4hdxw7i3m6q