2:15 PM - 2:30 PM
[PCG19-09] On the crystallinity of silicate dust in evolving protoplanetary disks due to magnetically driven disk winds
Keywords:Protoplanetary disk, Dust, Crystallinity, Magnetically driven disk wind
Understanding the process of radial mixing in protoplanetary disks is of great importance in the context of star and planet formation in the solar and extrasolar systems. In particular, the radial distribution of crystalline silicate dust particles in disks is the key to understanding the material mixing process from astronomical observations (e.g., Honda et al. 2006; Maaskant et al. 2015). In protoplanetary disks, dust particles are radially transported by three processes, namely, advection, diffusion, and the radial drift of dust particles. The effects of these processes in viscous accretion disks are studied so far (e.g., Gail 2001; Pavlyuchenkov & Dullemond 2007).
Recent observations of protoplanetary disks by ALMA revealed that the disk structure (e.g., rings, gaps, and spirals) formed in the early stage of disk evolution. The magnetically driven disk wind (e.g., Suzuki et al. 2010) is one of the candidates to create observed structures, and the effects of disk winds on the evolution of dust and gas are investigated in previous studies (e.g., Takahashi & Muto 2018).
Here we calculate the radial distribution of crystalline silicate dust particles in evolving protoplanetary disks due to magnetically driven disk winds. We found that the radial distribution of the crystallinity strongly depends on the timescales of viscous evolution, the radial drift of dust particles, and wind mass loss, as the structure of gas and dust also depends on these timescales (e.g., Takahashi & Muto 2018). The crystallinity of dust particles may relate to the structure of protoplanetary disks.
Recent observations of protoplanetary disks by ALMA revealed that the disk structure (e.g., rings, gaps, and spirals) formed in the early stage of disk evolution. The magnetically driven disk wind (e.g., Suzuki et al. 2010) is one of the candidates to create observed structures, and the effects of disk winds on the evolution of dust and gas are investigated in previous studies (e.g., Takahashi & Muto 2018).
Here we calculate the radial distribution of crystalline silicate dust particles in evolving protoplanetary disks due to magnetically driven disk winds. We found that the radial distribution of the crystallinity strongly depends on the timescales of viscous evolution, the radial drift of dust particles, and wind mass loss, as the structure of gas and dust also depends on these timescales (e.g., Takahashi & Muto 2018). The crystallinity of dust particles may relate to the structure of protoplanetary disks.