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dc.contributor.authorSousa, Alana P.
dc.contributor.authorAlencar, Silvia H. P.
dc.contributor.authorRebull, Luisa M.
dc.contributor.authorEspaillat, Catherine C.
dc.contributor.authorCalvet, Nuria
dc.contributor.authorTeixeira, Paula S.
dc.identifier.citationSousa , A P , Alencar , S H P , Rebull , L M , Espaillat , C C , Calvet , N & Teixeira , P S 2019 , ' A study of accretion and disk diagnostics in the NGC 2264 cluster ' , Astronomy & Astrophysics , vol. 629 , A67 .
dc.identifier.otherPURE: 261266958
dc.identifier.otherPURE UUID: 72ebc4f0-1609-4bff-a74e-a1c54228f6af
dc.identifier.otherRIS: urn:8AB1758C5B0A9C428C4DBC20C51E7772
dc.identifier.otherRIS: 10.105100046361201935563
dc.identifier.otherORCID: /0000-0002-3665-5784/work/61978988
dc.identifier.otherWOS: 000483925900002
dc.identifier.otherBibCode: 2019A&A...629A..67S
dc.identifier.otherScopus: 85103759373
dc.description.abstractContext. Understanding disk dissipation is essential for studying how planets form. Disk gaps and holes, which almost correspond to dust-free regions, are inferred from infrared observations of T Tauri stars (TTS), indicating the existence of a transitional phase between thick accreting disks and debris disks. Transition disks are usually referred to as candidates for newly formed planets. Aims. We searched for transition disk candidates belonging to NGC 2264. Using stellar and disk parameters obtained in the observational multiwavelength campaign CSI 2264, we characterized accretion, disk, and stellar properties of transition disk candidates and compared them to systems with a full disk and diskless stars. Methods. We modeled the spectral energy distribution (SED) of a sample of 401 TTS, observed with both CFHT equipped with MegaCam and IRAC instrument on the Spitzer, with Hyperion SED fitting code using photometric data from the U band (0.3 μm) to the Spitzer/MIPS 24 μm band. We used the SED modeling to distinguish transition disk candidates, full disk systems, and diskless stars. Results. We classified ∼52% of the sample as full disk systems, ∼41% as diskless stars, and ∼7% of the systems as transition disk candidates, among which seven systems are new transition disk candidates belonging to the NGC 2264 cluster. The sample of transition disk candidates present dust in the inner disk similar to anemic disks, according to the αIRAC classification, which shows that anemic disk systems can be candidate transition disks. We show that the presence of a dust hole in the inner disk does not stop the accretion process since 82% of transition disk candidates accrete and show Hα, UV excess, and mass accretion rates at the same level as full disk systems. We estimate the inner hole sizes, ranging from 0.1 to 78 AU, for the sample of transition disk candidates. In only ∼18% of the transition disk candidates, the hole size could be explained by X-ray photoevaporation from stellar radiation.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © ESO 2019. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at
dc.subjectStars: pre-main sequenceen
dc.subjectStars: variables: T Taurien
dc.subjectHerbig Ae/Been
dc.subjectAccretion disksen
dc.subjectProtoplanetary disksen
dc.subjectQB Astronomyen
dc.titleA study of accretion and disk diagnostics in the NGC 2264 clusteren
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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