Oral Presentation
The resolved dust gap-ring structure of the CR Cha disk and their possible origins
Presenter: Seongjoong Kim (Tokyo Institute of Technology)
Our recent ALMA observation has revealed the axisymmetric dust gap-ring structure r~100 au in the CR Cha protoplanetary disk. Meanwhile, the CO isotopologue (12CO, 13CO, and C18O) J = 2 − 1 emission lines toward the CR Cha protoplanetary disk shows a bump structure at ~ 130 au in the peak brightness temperature of 13CO line but not in 12CO. We investigate two possible mechanisms for reproducing the observed dust gap-ring structure and a gas temperature bump. First, the observed gap structure can be opened by a Jupiter mass planet using the relation between the planet mass and the gap depth and width. Meanwhile, the radiative transfer calculations based on the observed dust and gas surface density profile show that the observed dust ring could be formed by dust accumulation at the gas temperature bump, that is, the gas pressure bump produced beyond the outer edge of the dust disk.
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