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SUMMARY:The Impact of the Inner Dead Zone Interface on Numerical Simulatio
 ns of Protoplanetary Disks - Matthew Roberts\, DAMTP
DTSTART:20221110T130000Z
DTEND:20221110T140000Z
UID:TALK192527@talks.cam.ac.uk
CONTACT:Callum William Fairbairn
DESCRIPTION:The turbulent flows within protoplanetary disks (PPDs) regulat
 e accretion on to the central object and the assembly of solids and gas in
 to planets. Hence\, they are central to any study of our origins and of th
 e possibility of life outside the Solar System. \n\nThis talk will focus o
 n two key numerical simulations (one under the cylindrical approximation a
 nd one fully global) that explore key features which are present in the in
 ner regions of PPDs (roughly 0.03-5 au from the central star). This region
  encompasses the supposed habitable zone and research in this area is acce
 lerating at a rapid pace due to spectacular data in the (sub)-mm (e.g.\, A
 LMA\, SPHERE\, GRAVITY). Later this decade\, SKA will explore these inner 
 regions in even finer resolution.\n\nOne key feature of all models of the 
 inner regions of PPDs\, is that beyond a certain critical radius (~1 au)\,
  magnetohydrodynamic turbulence dies out on account of the sudden drop-off
  in thermal ionisation. The magnetorotational instability is swamped by th
 e abrupt rise in non-ideal effects and the gas beyond this critical radius
  is deemed ‘dead’. The mismatch of accretion across the transition (de
 ad zone interface) has several consequences for planet formation. First\, 
 a pressure bump develops that can trap and concentrate in-falling solid ma
 terial or inwardly migrating planets. Second\, the pressure bump is also s
 ubject to a Rossby wave instability that spawns vortices\, which in turn c
 oncentrates solid material further.
LOCATION:In Person MR12
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