On the multiple generations of planetary embryos

Abstract

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.

12 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics

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Cited by in corpus (11)

• The GAPS Programme with HARPS-N at TNG. XXXV. Fundamental properties of transiting exoplanet host stars
• Planetary Population Synthesis and the Emergence of Four Classes of Planetary System Architectures
• How to make giant planets via pebble accretion
• Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets
• Vertical shear instability in two-moment radiation-hydrodynamical simulations of irradiated protoplanetary disks I. Angular momentum transport and turbulent heating
• The interplay between pebble and planetesimal accretion in population synthesis models and its role in giant planet formation
• High Resolution Study of Planetesimal Formation by Gravitational Collapse of Pebble Clouds
• On the interaction of pebble accreting embryos with the gaseous disc: importance of thermal forces
• The New Generation Planetary Population Synthesis (NGPPS). VII. Statistical comparison with the HARPS/Coralie survey
• How does the chemical composition of solids influence the formation of planetesimals?
• Effects of Outer Giant Planets on In Situ Formation of Inner Super-Earths