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dc.contributor.authorKurtovic, N. T.
dc.contributor.authorPinilla, P.
dc.contributor.authorLong, F.
dc.contributor.authorBenisty, M.
dc.contributor.authorManara, C. F.
dc.contributor.authorNatta, A.
dc.contributor.authorPascucci, I.
dc.contributor.authorRicci, L.
dc.contributor.authorScholz, A.
dc.contributor.authorTesti, L.
dc.date.accessioned2021-02-26T12:30:15Z
dc.date.available2021-02-26T12:30:15Z
dc.date.issued2021-01
dc.identifier.citationKurtovic , N T , Pinilla , P , Long , F , Benisty , M , Manara , C F , Natta , A , Pascucci , I , Ricci , L , Scholz , A & Testi , L 2021 , ' Size and structures of disks around very low mass stars in the Taurus star-forming region ' , Astronomy and Astrophysics , vol. 645 , A139 . https://doi.org/10.1051/0004-6361/202038983en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 273003784
dc.identifier.otherPURE UUID: 2f7a39ef-75ca-4de1-abff-e7919556840d
dc.identifier.otherScopus: 85100451378
dc.identifier.otherWOS: 000614475100001
dc.identifier.urihttp://hdl.handle.net/10023/21516
dc.descriptionFunding Information: N.K. and P.P. acknowledge support provided by the Alexander von Humboldt Foundation in the framework of the Sofja Kovalevskaja Award endowed by the Federal Ministry of Education and Research. This Project has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 823823 (DUSTBUSTERS). This work was partly supported by the Deutsche Forschungs-Gemeinschaft (DFG, German Research Foundation) - Ref no. FOR 2634/1 TE 1024/1-1. T Open Access funding provided by Max Planck Society.en
dc.description.abstractContext. The discovery of giant planets orbiting very low mass stars (VLMS) and the recent observed substructu res in disks aroundVLMS is challenging planet formation models. Specifically, radial drift of dust particles is a catastrophic barrier in these disks, which prevents the formation of planetesimals and therefore planets.  Aims. 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. Methods. We studied six disks around VLMS in the Taurus star-forming region using ALMA Band 7 (340 GHz) at a resolution of 0:100. The targets were selected because of their high disk dust content in their stellar mass regime.  Results. Our observations resolve the disk dust continuum in all disks. In addition, we detect the 12CO (J = 3) emission line in all targets and 13CO (J = 32) 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 MHO6 (M 5.0) and CIDA1 (M 4.5), while we have a tentative detection of a multi-ringed disk around J0433. We estimate that a planet mass of 0:1 MJup or 0:4 MSaturn is required for a single planet to create the first gap in J0433. For the cavities of MHO6 and CIDA1, a Saturn-mass planet (0.3 MJup) is required. The other three disks with no observed structures are the most compact and faintest in our sample, with the radius enclosing 90% of the continuum emission varying between 13 and 21 au. 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 Rgas, the ratio of Rgas=Rdust in our sample varies from 2.3 to 6.0. One of the disks in our sample, CIDA7, has the largest Rgas=Rdust ratio observed so far, which is onsistent with models of radial drift being very efficient around VLMS in the absence of substructures. Conclusions. Given our limited angular resolution, substructures were only directly detected in the ost extended disks, which represent 50% of our sample, and there are hints of unresolved structured emission in one of the bright smooth sources. 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.
dc.format.extent23
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysicsen
dc.rightsCopyright © N. T. Kurtovic et al. 2021. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSize and structures of disks around very low mass stars in the Taurus star-forming regionen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202038983
dc.description.statusPeer revieweden


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