Resolved millimeter-dust continuum cavity around the very low mass young star CIDA 1
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Context. Transition disks (TDs) are circumstellar disks with inner regions highly depleted in dust. TDs are observed in a small fraction of disk-bearing objects at ages of 1-10 Myr. They are important laboratories to study evolutionary effects in disks, from photoevaporation to planet-disk interactions. Aims. We report the discovery of a large inner dust-empty region in the disk around the very low mass star CIDA 1 (M* ~0.1-0.2 M⊙). Methods. We used ALMA continuum observations at 887 μm, which provide a spatial resolution of 0." 21 x 0." 12(~15x8 au in radius at 140pc). Results. The data show a dusty ring with a clear cavity of radius ~20 au, the typical characteristic of a TD. The emission in the ring is well described by a narrow Gaussian profile. The dust mass in the disk is ~17 M⊕. CIDA 1 is one of the lowest mass stars with a clearly detected millimeter cavity. When compared to objects of similar stellar mass, it has a relatively massive dusty disk (less than ~5% of Taurus Class II disks in Taurus have a ratio of Mdisk/M* larger than CIDA 1) and a very high mass accretion rate (CIDA 1 is a disk with one of the lowest values of Mdisk/M ever observed). In light of these unusual parameters, we discuss a number of possible mechanisms that can be responsible for the formation of the dust cavity (e.g.,photoevaporation, dead zones, embedded planets, close binary). We find that an embedded planet of a Saturn mass or a close binary are the most likely possibilities.
Pinilla , P , Natta , A , Manara , C F , Ricci , L , Scholz , A & Testi , L 2018 , ' Resolved millimeter-dust continuum cavity around the very low mass young star CIDA 1 ' , Astronomy & Astrophysics , vol. 615 . https://doi.org/10.1051/0004-6361/201832690
Astronomy & Astrophysics
© 2018, ESO. This work has been made available online in accordance with the publisher’s policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201832690
DescriptionFunding: ERC grant 743029 EASY.
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