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dc.contributor.authorPinilla, Paola
dc.contributor.authorNatta, Antonella
dc.contributor.authorManara, Carlo F.
dc.contributor.authorRicci, Luca
dc.contributor.authorScholz, Aleks
dc.contributor.authorTesti, Leonardo
dc.date.accessioned2018-07-05T12:30:07Z
dc.date.available2018-07-05T12:30:07Z
dc.date.issued2018-07-01
dc.identifier.citationPinilla , 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/10.1051/0004-6361/201832690en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 253378804
dc.identifier.otherPURE UUID: 08913cd2-4c0b-4dff-bf73-b2d2ef5e1174
dc.identifier.otherBibCode: 2018arXiv180500960P
dc.identifier.otherBibCode: 2018A&A...615A..95P
dc.identifier.otherScopus: 85060772230
dc.identifier.otherWOS: 000439526600004
dc.identifier.urihttps://hdl.handle.net/10023/14988
dc.descriptionFunding: ERC grant 743029 EASY.en
dc.description.abstractContext. 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.
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 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/10.1051/0004-6361/201832690en
dc.subjectAccretionen
dc.subjectAccretion disken
dc.subjectCircumstellar matteren
dc.subjectStars: premain-sequence-protoplanetary-disk-formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleResolved millimeter-dust continuum cavity around the very low mass young star CIDA 1en
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPostprinten
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/10.1051/0004-6361/201832690
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1805.00960en
dc.identifier.grantnumberST/M001296/1en


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