Constraining dust properties of planet-forming disks at high angular resolution is fundamental to understand how solids are trapped at the location of substructure, and how dust growth could be favored or accelerated therein.
Millimeter observations with ALMA are capable of resolving scales down to few astronomical units, enough to infer the differences between the dust properties in these substructures and the rest of the disk.
Here, we use ALMA dust continuum observations of the disks around AS209, GMAur, HD163296, IMLup, and MWC480 and explore a large parameter space to constrain the radial distribution of solid mass and maximum grain size that can explain the spatially-resolved spectrum of each disk.
In general, we find that the dust surface density and grain size profiles decrease from the inner disks to the outer disks, with local maxima at the bright rings locations, as expected from dust trapping models. The inferred grain sizes from the inner to outer disks vary from ~1 cm to 1 mm.
Finally, based on the estimated Toomre parameter, the disks are found to be gravitationally stable, except IMLup, which has a Toomre parameter below 2 at radii >~ au.
Virtual room: https://uchile.zoom.us/j/81365909464?pwd=aFYva3JpSXZUYnd0Z3o2OVZ6OS9GQT09
Ver presentación: Presentación Anibal Sierra