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dc.contributor.authorKeane, J.T.
dc.contributor.authorPascucci, I.
dc.contributor.authorEspaillat, C.
dc.contributor.authorWoitke, P.
dc.contributor.authorAndrews, S.
dc.contributor.authorKamp, I.
dc.contributor.authorThi, W.-F.
dc.contributor.authorMeeus, G.
dc.contributor.authorDent, W.R.F.
dc.date.accessioned2014-08-29T12:01:03Z
dc.date.available2014-08-29T12:01:03Z
dc.date.issued2014-06-01
dc.identifier.citationKeane , J T , Pascucci , I , Espaillat , C , Woitke , P , Andrews , S , Kamp , I , Thi , W-F , Meeus , G & Dent , W R F 2014 , ' Herschel evidence for disk flattening or gas depletion in transitional disks ' , Astrophysical Journal , vol. 787 , no. 2 . https://doi.org/10.1088/0004-637X/787/2/153en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 144262198
dc.identifier.otherPURE UUID: 8f09d982-587c-4037-bcc0-fad186182140
dc.identifier.otherScopus: 84901020703
dc.identifier.otherWOS: 000336246700058
dc.identifier.urihttp://hdl.handle.net/10023/5296
dc.descriptionI.P., J.T.K., C.E., and S.A. acknowledge NASA/JPL for funding support.en
dc.description.abstractTransitional disks are protoplanetary disks characterized by reduced near- and mid-infrared emission, with respect to full disks. This characteristic spectral energy distribution indicates the presence of an optically thin inner cavity within the dust disk believed to mark the disappearance of the primordial massive disk. We present new Herschel Space Observatory PACS spectra of [O I] 63.18 μm for 21 transitional disks. Our survey complements the larger Herschel GASPS program ("Gas in Protoplanetary Systems") by quadrupling the number of transitional disks observed with PACS in this wavelength. [O I] 63.18 μm traces material in the outer regions of the disk, beyond the inner cavity of most transitional disks. We find that transitional disks have [O I] 63.18 μm line luminosities ∼2 times fainter than their full disk counterparts. We self-consistently determine various stellar properties (e.g., bolometric luminosity, FUV excess, etc.) and disk properties (e.g., disk dust mass, etc.) that could influence the [O I] 63.18 μm line luminosity, and we find no correlations that can explain the lower [O I] 63.18 μm line luminosities in transitional disks. Using a grid of thermo-chemical protoplanetary disk models, we conclude that either transitional disks are less flared than full disks or they possess lower gas-to-dust ratios due to a depletion of gas mass. This result suggests that transitional disks are more evolved than their full disk counterparts, possibly even at large radii.
dc.format.extent24
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectAccretionen
dc.subjectAccretion disksen
dc.subjectCircumstellar matteren
dc.subjectInfrared: starsen
dc.subjectProtoplanetary disksen
dc.subjectStars: pre-main sequenceen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleHerschel evidence for disk flattening or gas depletion in transitional disksen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/787/2/153
dc.description.statusPeer revieweden


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