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SUMMARY:Planet formation by pebble accretion - Dr Michiel Lambrechts
DTSTART:20220523T130000Z
DTEND:20220523T140000Z
UID:TALK173375@talks.cam.ac.uk
CONTACT:Callum William Fairbairn
DESCRIPTION:Surveys of star-forming regions show that protoplanetary gas d
 iscs around young stars contain most of their solid mass in particles that
  are approximately mm in size. If left unperturbed\, these so-called pebbl
 es will drift radially towards the host star\, on time-scales of a few Myr
 \, because of the drag they experience with respect to the surrounding gas
 . As a consequence\, planet formation becomes a race against time. This ta
 lk will focus on how these pebbles are the main building blocks of planet 
 formation. First\, spontaneous pile-ups of pebble swarms\, triggered by st
 reaming instabilities\, can form asteroid-sized objects called planetesima
 ls. Thereafter\, the largest of these planetesimals can efficiently sweep 
 up the surrounding drifting pebbles\, by a process called pebble accretion
 . In this way\, the massive cores of the gas-giant planets can form in orb
 its outside the water ice line. Furthermore\, within the ice line\, we sho
 w that the outcome of planet formation results in either terrestrial-like 
 planets or super-Earth systems\, based N-body simulations that include pla
 net growth by pebble accretion and planetary migration. These new theoreti
 cal finding will be placed in the context of the observed diversity in exo
 planets and recent cosmochemical findings in the Solar System that are ind
 icative of large-scale pebble drift.
LOCATION:In Person MR14
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