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We have carried out two-dimensional hydrodynamical simulations to study theeffects of disk self-gravity and radiative cooling on the formation of gaps andspirals. (1) With disk self-gravity included, we find stronger, moretightly-wound spirals and deeper gaps in more massive disks. The deeper gapsare due to the larger Angular Momentum Flux (AMF) of the waves excited in moremassive disks, as expected from the linear theory. The position of thesecondary gap does not change, provided that the disk is not extremely massive($Q \gtrsim 2$). (2) With radiative cooling included, the excited spiralsbecome monotonically more open (less tightly-wound) as the disk's coolingtimescale increases. On the other hand, the amplitude and strength of thespirals decrease when the cooling time increases from a small value to $\sim1/\Omega$, but then the amplitude starts to increase again when the coolingtime continues to increase. This indicates that radiative dissipation becomesimportant for waves with $T_{cool}\sim$ 1. Consequently, the induced primarygap is narrower and the secondary gap becomes significantly shallower when thecooling time becomes $\sim 1/\Omega$. When the secondary gap is present, theposition of it moves to the inner disk from the fast cooling cases to the slowcooling cases. The dependence of gap properties on the cooling timescale (e.g.in AS 209) provides a new way to constrain the disk optical depth and thus disksurface density.

The effects of disk self-gravity and radiative cooling on the formation of gaps and spirals by young planets