学术文献库

Global models of planet formation tend to begin with an initial set of planetary embryos for the sake simplicity. While this approach gives valuable insights on the evolution of the initial embryos, the initial distribution itself is a bold assumption. Limiting oneself to an initial distribution may neglect essential physics that precedes, or follows said initial distribution. We wish to investigate the effect of dynamic planetary embryo formation on the formation of planetary systems. The presented framework begins with an initial disk of gas, dust and pebbles. The disk evolution, the formation of planetesimals and the formation of planetary embryos is modeled consistently. Embryos then grow by pebble, planetesimal and eventually gas accretion. Planet disk interactions and N-body dynamics with other simultaneously growing embryos is included in the framework. We show that the formation of planets can occur in multiple consecutive phases. Earlier generations grow massive by pebble accretion but are subject to fast type I migration and thus accretion to the star. The later generations of embryos that form grow to much smaller masses by planetesimal accretion, as the amount of pebbles in the disk has vanished. The formation history of planetary systems may be far more complex than an initial distribution of embryos could reflect. The dynamic formation of planetary embryos needs to be considered in global models of planet formation to allow for a complete picture of the systems evolution.