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SUMMARY:Magnetorotational turbulence and dust dynamics in the inner region
 s of protoplanetary discs - Thomas Jannaud (DAMTP Cambridge)
DTSTART:20260129T123000Z
DTEND:20260129T133000Z
UID:TALK243625@talks.cam.ac.uk
CONTACT:Mika Kontiainen
DESCRIPTION:The magnetorotational instability (MRI) plays a crucial role i
 n the evolution of many types of accretion discs. It controls the accretio
 n onto the central object by driving turbulence\, but also enables the lau
 nching of magnetised winds and jets. The MRI is most often studied using i
 deal magnetohydrodynamic (MHD) simulations of accreting discs. I will firs
 t present some generic results on the MRI and some issues with its use in 
 MHD simulations.\nI will then focus on the peculiar case of protoplanetary
  discs. Their study has seen tremendous progress in the past decades\, spe
 arheaded by many observations in the radio and infrared bands (ALMA\, SPHE
 RE\, GRAVITY...). In the inner regions of those discs lies a transition be
 tween an inner\, MRI-turbulent zone\, and an outer\, laminar zone. This tr
 ansition is a prime location for the accumulation of solids contained in t
 he disc. That accumulation is of particular interest\, as it is the first 
 step of planet formation. I will show results extracted from 3D global MHD
  simulations of the inner regions of protoplanetary discs. Those simulatio
 ns include non-ideal MHD effects and the presence of solids. They show a q
 uick pileup of dust at the aforementioned transition. I will also highligh
 t the influence of magnetised winds\, as well as that of vortices induced 
 by the Rossby-Wave Instability.\n\n
LOCATION:Institute of Astronomy 
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