= Accretion-disk self-gravity
\b[Accretion-disk self-gravity] is the contribution of the disk's own matter to its gravitational field. A low total disk mass can still matter for local vertical confinement or the growth of density disturbances. The <Toomre parameter> compares gravity with <pressure> and rotation, but instability does not guarantee fragmentation: heating by gravitationally driven motions can balance cooling. Local numerical experiments distinguish that regulated state from breakup when cooling is sufficiently rapid.<Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks by Charles F. Gammie>[Abstract: self-regulated gravitational turbulence versus fragmentation in a local cooling model]{ref}
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