The detection of dust gap-ring structure in the outer region of the CR Cha protoplanetary disk

Abstract

We observe the dust continuum at 225 GHz and CO isotopologue (12CO, 13CO, and C18O) J=2-1 emission lines toward the CR Cha protoplanetary disk using the Atacama Large Millimeter/Submillimeter Array (ALMA). The dust continuum image shows a dust gap-ring structure in the outer region of the dust disk. A faint dust ring is also detected around 120 au beyond the dust gap. The CO isotopologue lines indicate that the gas disk is more extended than the dust disk. The peak brightness temperature of the 13CO line shows a small bump around 130 au while 12CO and C18O lines do not show. 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 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.

21 pages, figures

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• On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
• No Significant Correlation between Line-emission and Continuum Substructures in the Molecules with ALMA at Planet-forming Scales Program
• DBNets: A publicly available deep learning tool to measure the masses of young planets in dusty protoplanetary discs
• ALMA observation of the protoplanetary disk around WW Cha: faint double-peaked ring and asymmetric structure
• Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants
• Multiple Rings and Asymmetric Structures in the Disk of SR 21