Abstract
We show that different physical mechanisms drive the m=1 gravitational instability for high and low disk masses. For high disk masses, sling amplification is dominant. For low disk masses, swing amplification and the indirect potential are both important. In any case, the m=1 mode is sensitive to the outer boundary condition. The dependence of the swing amplification on Toomre's Q parameter is somewhat reduced by the fact that the distance between the corotation point and the outer disk edge decreases as the disk mass decreases
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