Gravitational instability in protoplanetary disk with cooling: 2D global analysis

Abstract

Self-gravity is important in protoplanetary disks for planet formation through gravitational instability (GI). We study the cooling effect on GI in a thin two-dimensional protoplanetary disk. By solving the linear perturbation equations in global geometry, we obtain all the normal modes. Faster cooling leads to faster growth rate of GI with lower azimuthal wavenumber $m$. According to the spatial structure of normal modes at different mass-averaged Toomre number $\overline{Q}$ and dimensionless cooling timescale $\beta$, we identify three modes: local, transitional and global. The transitional modes are located in the outer disk while the other two modes in the inner disk. At $\beta\approx 1$ (the resonance of dynamical timescale and thermal timescale) the growth rate changes sharply and the transitional modes dominate. The disk $\alpha$ due to GI is much higher in the transitional modes than in the other two. Our result implies that the transitional modes at $\overline{Q}\approx 1$ and $\beta\approx 1$ can plausibly interpret the substructures and planet/brown dwarf formation in the outer disk.