Spatial distribution of crystalline silicates in protoplanetary disks: How to interpret JWST observations

Crystalline silicate is an important tracer for the evolution of dust, the main building block of planet formation. In an inner protoplanetary disk, amorphous silicates are annealed by the high temperature and form crystalline silicates. These crystalline silicates are radially and vertically distributed by disk turbulence, radial drift, and radial diffusion. In this project, we study how the distributed crystalline silicates affect mind-infrared observation from the MIRI in the recently launched JWST. The MIRI can observe the inner protoplanetary disks in mid-infrared wavelength but only the upper layer due to the optically thick disk. Thus, we also study how the MIRI observation represents the crystalline silicates in the midplane, where planets are mainly formed. From the comparison between radial and vertical distribution timescales, we conclude crystalline silicates in an observation well represent the midplane. In our modeled T-Tauri disk, different sizes of dust get crystallized in different ranges of the inner disk and distributed up to a few AU by the radial transport. As the results, the spatial distribution affects feature strengths in mid-infrared wavelength