Forming Planets via Pebble Accretion

By Anders Johansen, Michiel Lambrechts. 2017

285 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/15d6ec6be8842b156dd284b9604ec543e10d89a1

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Citations in the corpus

Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “We note that the disk region most directly relevant to planet formation according to planet formation models is the inner 10s of au of the disk midplane (e.g., Pollack et al. 1996; Raymond et al. 2014; Johansen & Lambrechts 2017).”
The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au (2019, methodology): “We update this reasoning within the emerging paradigm of “pebble accretion,” in which cores grow by accreting small solid particles aerodynamically entrained in disk gas (see Ormel 2017 and Johansen & Lambrechts 2017 for reviews).”
Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, background): “In scenarios like pebble accretion (e.g., Johansen et al. 2007; Johansen & Lambrechts 2017; Ormel 2017), for example, only a small fraction of the pebble flux is captured by growing planets (see Guillot et al. 2014).”
Astrochemistry and compositions of planetary systems (2020, background): “(2018); Laas and Caselli (2019); Le Gal et al.”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, background): “…largest planetesimals have grown to a few hundred kilometers in size by accreting other planetesimals, rapid pebble accretion allows further growth to cores of ten Earth masses well within the lifetime of the protoplanetary disc (Ida et al. 2016; Visser & Ormel 2016; Johansen & Lambrechts 2017).”