On the evolution of pebble-accreting planets in evolving protoplanetary discs

ABSTRACT We examine the migration of luminous low-mass cores in laminar protoplanetary discs where accretion occurs mainly because disc winds and planet luminosity is generated by pebble accretion. Using 2D hydrodynamical simulations, we determine eccentricities induced thermal forces as a function gas rates, also evaluate importance torque exerted solid component relative to torque. For rate $\dot{M}= 2\times 10^{-8}\, \mathrm{ M}_\odot$ yr−1 flux $\dot{M}_{\mathrm{ peb}}=170\, M}_\oplus$ Myr−1, find that embryo attain values comparable aspect ratio. The radial excursion disc, however, causes inflowing pebbles cancel on average transition from outward inward. This found arise magnitude torques decreases exponentially with increasing eccentricity, provide fitting formula for attenuation eccentricity. As evolves, becomes at some point too small make core eccentricity grow such can exert non-zero planet. positive rates $\dot{M} \lesssim 5\times 10^{-9}$M⊙ fluxes $\dot{M}_{\rm {peb}} 120\, M}_\oplus $ it overcome mass $m_\mathrm{ p}\lesssim \, 1\,\mathrm{ {M}}_\oplus$, resulting migration.