Evolution of eccentricity and inclination of hot protoplanets embedded in radiative discs

We study the evolution of the eccentricity and inclination of protoplanetary embryos and low-mass protoplanets (from a fraction of an Earth mass to a few Earth masses) embedded in a protoplanetary disc, by means of three-dimensional hydrodynamics calculations with radiative transfer in the diffusion limit. When the protoplanets radiate in the surrounding disc the energy released by the accretion of solids, their eccentricity and inclination experience a growth towards values that depend on the luminosity-to-mass ratio of the planet, which are comparable to the disc's aspect ratio and which are reached over time-scales of a few thousand years. This growth is triggered by the appearance of a hot, underdense region in the vicinity of the planet. The growth rate of the eccentricity is typically three times larger than that of the inclination. In long-term calculations, we find that the excitation of eccentricity and the excitation of inclination are not independent. In the particular case in which a planet has initially a very small eccentricity and inclination, the eccentricity largely overruns the inclination. When the eccentricity reaches its asymptotic value, the growth of inclination is quenched, yielding an eccentric orbit with a very low inclination. As a side result, we find that the eccentricity and inclination of non-luminous planets are damped more vigorously in radiative discs than in isothermal discs.