Speaker
Description
Protoplanetary disks (PPD) have been widely observed around young stars and are supposed to host planetary formation. Among these disks stand the transition disks (TD) which are characterized by a large hole in the central regions, whose formation remains yet unexplained. Despite this hole, accretion rates comparable to the ones found in PPD are measured, suggesting an inward motion of matter.
A possible explanation for these high accretion rates is the presence of magnetised winds that would allow matter to fall onto the star at high radial velocity. Following previous works, the disk can be described using non ideal MHD while the ideal MHD picture is used to compute the wind.
I will show the impact of the depleted dust repartition in TDs on the ionization fraction through theoretical calculations based on a simple lattice of chemical reactions. It can be shown that the non ideal MHD effects are also affected by such a hole. I will then present the results of 2D simulations modelling winds in a TD based on the predicted non ideal effects profiles.
Axisymetry allows to explore the parameters space and to check the stability of the hole profile through time. Such a work will later on lead the way to a more accurate description of the chemistry at stake in TD and 3D simulations.
