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"Debris disks" around young stars (analogues of the Kuiper Belt in our SolarSystem) show a variety of non-trivial structures attributed to planetaryperturbations and used to constrain the properties of the planets. However,these analyses have largely ignored the fact that some debris disks are foundto contain small quantities of gas, a component that all such disks shouldcontain at some level. Several debris disks have been measured with adust-to-gas ratio around unity at which the effect of hydrodynamics on thestructure of the disk cannot be ignored. Here we report linear and nonlinearmodelling that shows that dust-gas interactions can produce some of the keypatterns attributed to planets. We find a robust clumping instability thatorganizes the dust into narrow, eccentric rings, similar to the Fomalhautdebris disk. The conclusion that such disks might contain planets is notnecessarily required to explain these systems.

Formation of sharp eccentric rings in debris disks with gas but without planets