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SUMMARY:From gas turbulence to planets: the formation of rocky planets at 
 the dead-zone inner edge. - Mario Flock - MPIA
DTSTART:20220426T120000Z
DTEND:20220426T130000Z
UID:TALK172481@talks.cam.ac.uk
CONTACT:Dr Mathias Nowak
DESCRIPTION:\nThe research of how planets form is one of the key branches 
 in astrophysics. Planet formation takes place in the so called proto-plane
 tary disk\, an accretion disk which establishes after the collapse of a mo
 lecular cloud.  99 per cent of the disk mass consists out of hydrogen and 
 helium gas while only one percent is stored in granular matter in form of 
 dust grains. Gas turbulence controls not only the evolution of the proto-p
 lanetary disk. The turbulent motion determines how fast the dust grains co
 llide and where they can grow to pebbles and planetesimals\, the first bui
 lding blocks of planets. \n\nIn my talk I will present state-of-the-art 3D
  radiative non-ideal magneto-hydrodynamical simulations of the gas and the
  dust component in protoplanetary disks. The simulation results reveal the
  detailed gas and dust dynamics\, including the regions with active magnet
 o-rotational instability and the locations for which we expect dust pebble
 s to concentrate and grow. The results demonstrate the important role of t
 he ionization transition zones as formation sides of planets in the disk. 
 Finally I summarize how we can further benefit from our models as we compa
 re them to recent disk observations and outline the next big steps\, neede
 d to advance in our understanding how and where planets form.\n\n\n
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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