Papers › Size and structures of disks around very low mass stars in the Taurus star-forming region
Size and structures of disks around very low mass stars in the Taurus star-forming region
Nicolas T. Kurtovic, Paola Pinilla, Feng Long, Myriam Benisty, Carlo F. Manara, Antonella Natta, Ilaria Pascucci, Luca Ricci, Alexander Scholz, Leonardo Testi
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We aim to estimate if structures, such as cavities, rings, and gaps, are common in disks around VLMS and to test models of structure formation in these disks. We also aim to compare the radial extent of the gas and dust emission in disks around VLMS, which can give us insight about radial drift. We studied six disks around VLMS in the Taurus star-forming region using ALMA Band 7 (∼340GHz) at a resolution of ∼0.1″. The targets were selected because of their high disk dust content in their stellar mass regime. Our observations resolve the disk dust continuum in all disks. In addition, we detect the ¹²CO (J=3-2) emission line in all targets and ¹³CO (J=3-2) in five of the six sources. The angular resolution allows the detection of dust substructures in three out of the six disks, which we studied by using UV-modeling. Central cavities are observed in the disks around stars MHO\,6 (M5.0) and CIDA\,1 (M4.5), while we have a tentative detection of a multi-ringed disk around J0433. Single planets of masses 0.1∼0.4 M_(Jup) would be required. The other three disks with no observed structures are the most compact and faintest in our sample. The emission of ¹²CO and ¹³CO is more extended than the dust continuum emission in all disks of our sample. When using the ¹²CO emission to determine the gas disk extension R_(gas), the ratio of R_(gas)/R_(dust) in our sample varies from 2.3 to 6.0, which is consistent with models of radial drift being very efficient around VLMS in the absence of substructures. Our observations do not exclude giant planet formation on the substructures observed. A comparison of the size and luminosity of VLMS disks with their counterparts around higher mass stars shows that they follow a similar relation.
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