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SUMMARY:Pebble accretion in turbulent discs
DTSTART;VALUE=DATE-TIME:20200514T115500Z
DTEND;VALUE=DATE-TIME:20200514T121500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-45@meetings.aip.de
DESCRIPTION:Speakers: Giovanni Picogna (Universitäts-Sternwarte München\
 , LMU)\nPlanets are born in the mid-plane of accretion discs around young 
 protostars. This process takes place most likely in weakly ionised regions
 \, where the evolution of the environment is driven by internal turbulence
  and the gas flow is not laminar but has stochastic components. Turbulence
  can be generated purely hydrodynamically via different instabilities\, li
 ke the vertical shear instability (VSI). A fast pathway to the formation o
 f giant planetary cores has been recently identified in pebble accretion\,
  though a realistic investigation of this process in a turbulent environme
 nt was necessary. We tested the solid accretion of a large range of dust s
 izes on to different planetary core masses in a VSI turbulent global 3D di
 sc and compared it with a laminar disc. Furthermore\, we tested the influe
 nce of a realistic equation of state and radiative cooling on the efficien
 cy of pebble accretion. We found that turbulence decreases slightly the so
 lid accretion efficiency with respect to analytical calculations of lamina
 r discs\, having a ~2% efficiency of pebble-like particles for a 5 Earth-m
 ass planet at 5 au. The introduction of radiative transfer can affect this
  result significantly by changing the aspect ratio of the disc\, thus the 
 pebble isolation mass.\n\nhttps://meetings.aip.de/event/1/contributions/45
 /
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/45/
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