Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study

ABSTRACT By means of three-dimensional high-resolution hydrodynamical simulations, we study the orbital evolution weakly eccentric or inclined low-mass protoplanets embedded in gaseous discs subject to thermal diffusion. We consider both non-luminous planets and that also experience radiative feedback from their own luminosity. compare our results previous analytical work find forces (the contribution disc’s force arising effects) match those predicted by linear theory within ?20 per cent. When planet’s luminosity exceeds a threshold found be 10 cent theory, its eccentricity inclination grow exponentially, whereas these quantities undergo strong damping below this threshold. In regime low indeed, diffusion cools surroundings planet allows gas accumulate vicinity. It is dynamics excess contributes damp inclination. The rates obtained can up h?1 times larger than due resonant interaction with disc, where h aspect ratio. This suggests models incorporate planet–disc interactions using well-known formulae based on wave-launching describe underestimate action disc an order magnitude.