 Inviscid warp equations of a nearly Keplerian disk

Here $G$ is the complex internal horizontal torque, $P$ the vertically integrated pressure, and ${\omega }_1,{\omega }_2$ the approximate nodal precession and apsidal precession rates. In the exactly Keplerian case, local plane waves obey ${\omega }^2=k^{2}P/(4\Sigma )=k^2{c}_s^2/4$, so tilt disturbances propagate at $c_s/2$. The secular thin-disk approximation requires wavelengths large relative to the height while the local approximation requires them small relative to the orbital radius.