Abstract
Planets can carve gaps in the surface density of protoplanetary discs. The formation of these gaps can reduce the corotation torques acting on the planets.
In addition, gaps can halt the accretion of solids on to the planets as dust and pebbles can be trapped at the edge of the gap. This accumulation of dust could explain the origin of the ring-like dust structures observed using high-resolution interferometry.
In this work, we provide an empirical scaling relation for the depth of the gap cleared by a planet on an eccentric orbit as a function of the planet-to-star mass ratio q, the disc aspect ratio h, Shakura-Sunyaev viscosity parameter alpha, and planetary eccentricity e. We construct the scaling relation using a heuristic approach: we calibrate a toy model based on the impulse approximation with 2D hydrodynamical simulations.
The scaling reproduces the gap depth for moderate eccentricities (e <= 4h) and when the surface density contrast outside and inside the gap is <= 10(2). Our framework can be used as the basis of more sophisticated models aiming to predict the radial gap profile for eccentric planets.