摘要：In the planet formation simulations presented in Bitsch et al. (2015b) a programming error led to an overestimate of the column density of pebbles. Correcting this error results in pebble column densities <0.1 g cm−2 at 10 AU after 1 Myr of protoplanetary disc evolution – significantly lower than observed pebble column densities in protoplanetary discs. As a consequence, the pebble accretion rates of growing protoplanets are lowered significantly. We demonstrate here how a revised model for the formation of pebbles in protoplanetary discs produces pebble surface densities more consistent with observations. The revised model assumes that the outer regions of protoplanetary discs are not depleted by mass accretion onto the star, which results in a significant increase in the pebble flux through the inner disc. Using this model, the conclusions of Bitsch et al. (2015b) remain unchanged: pebble accretion accelerates the growth of cores in the outer disc to out-compete planetary migration, yielding final orbits that are consistent with cold gas giants in the solar system as well as in exoplanetary systems.
关键词：enaccretion, accretion disksplanets and satellites: formationprotoplanetary disksplanet-disk interactionserrata, addenda
