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SUMMARY:Formation of planetary cores in spontaneously generated dust traps
  during the secular evolution of magnetized protoplanetary disks - Timmy D
 elage (Imperial)
DTSTART:20250429T120000Z
DTEND:20250429T130000Z
UID:TALK231337@talks.cam.ac.uk
CONTACT:Dr Dolev Bashi
DESCRIPTION:An outstanding gap in the current planet formation theory is a
 bout the first steps of the planet formation process\; namely how\, when a
 nd where the initially ISM like solid dust particles grow into pebbles and
  planetesimals\, the building blocks of planetary cores. Protoplanetary di
 sks provide the initial conditions for the planet formation process. They 
 are weakly magnetized accretion disks that are subject to the magnetorotat
 ional instability (MRI)\, one of the main magnetized processes responsible
  for their angular momentum transport and gas turbulence. The nonideal mag
 netohydrodynamic (MHD) effects prevent the MRI from operating everywhere i
 n PPDs\, leading to a complex dichotomy between MRI active regions with hi
 gher gas turbulence and non-MRI regions with lower gas turbulence. In this
  talk\,  I will present the first numerical framework that describes the 
 evolution of PPDs over millions of years powered by the MRI. It captures t
 he MRI driven gas evolution via nonideal MHD calculations\, which accounts
  for the dynamics and growth of the solid dust particles. An MRI powered m
 echanism that can spontaneously generate short- and long-lived pressure ma
 xima in the PPD is unveiled. Within the long-lived pressure maxima\, solid
  dust particles can be efficiently trapped\, grow into pebbles\, and reach
  high enough dust-to-gas mass ratios to potentially trigger the formation 
 of planetesimals via the streaming instability. These planetesimals and pe
 bbles can further rapidly interact to form planetary cores.
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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