Forming Planets via Pebble Accretion

    Forskningsoutput: TidskriftsbidragArtikel i vetenskaplig tidskriftPeer review

    Sammanfattning

    The detection and characterization of large populations of pebbles in protoplanetary disks have motivated the study of pebble accretion as a driver of planetary growth. This review covers all aspects of planet formation by pebble accretion, from dust growth over planetesimal formation to the accretion of protoplanets and fully grown planets with gaseous envelopes. Pebbles are accreted at a very high rate-orders of magnitude higher than planetesimal accretion-and the rate decreases only slowly with distance from the central star. This allows planetary cores to start their growth in much more distant positions than their final orbits. The giant planets orbiting our Sun and other stars, including systems of wide-orbit exoplanets, can therefore be formed in complete consistency with planetary migration. We demonstrate how growth tracks of planetary mass versus semimajor axis can be obtained for all the major classes of planets by integrating a relatively simple set of governing equations.

    Originalspråkengelska
    Sidor (från-till)359-387
    Antal sidor29
    TidskriftAnnual Review of Earth and Planetary Sciences
    Volym45
    DOI
    StatusPublished - 2017 aug. 30

    Ämnesklassifikation (UKÄ)

    • Astronomi, astrofysik och kosmologi

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