Structure of the protoplanetary disk around V1094 Sco obtained from dust
continuum emission and SED

Speaker: Sanemichi Takahashi (NAOJ)


Recent ALMA observations have found that detailed structures are formed in protoplanetary disks. Understanding the structure of protoplanetary disks is important for revealing the environment of planet formation. In this work, we investigate the structure of the protoplanetary disk around V1094 Sco. The previous study indicates that the disk around V1094 Sco is cold and massive according to its spectral energy distribution (Tsukagoshi et al. 2011). Moreover, ALMA observations at Band 6 and 7 found that two ring structures are formed in the disk (van Terwisga et al. 2018). To understand the physical nature of the disk, we investigated its temperature and surface density distributions using our ALMA observation data of the dust continuum at Band 8 and SED, and compared them with the radiative transfer calculations. According to the dust continuum emission at Band 8, we found that the disk consists of two regions, inner bright region (< 100 au) and outer dark plateau (>100 au), in which the radial profile of the intensity is shallower than the inner bright region.  Our radiative transfer calculations indicate that the inner region is optically thick and the outer plateau is optically thin. The radiative transfer calculations also suggest that the small grains are depleted or settle to the midplane in the disk to reproduce SED. This result suggests that the dust grains grow or the turbulence is weak in the disk of V1094 Sco.