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dc.creatorOliveira, Isaen_US
dc.creatorMerin, Brunoen_US
dc.creatorPontoppidan, Klaus M.en_US
dc.creatorvan Dishoeck, Ewine F.en_US
dc.date.accessioned2016-04-28T19:33:38Z
dc.date.available2016-04-28T19:33:38Z
dc.date.issued2013-01en
dc.identifierdoi:10.15781/T21Z35
dc.identifier.citationOliveira, Isa, Bruno Mer�n, Klaus M. Pontoppidan, and Ewine F. Van Dishoeck. "The physical structure of protoplanetary disks: the Serpens cluster compared with other regions." The Astrophysical Journal 762, no. 2 (Jan., 2013): 128.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34741
dc.description.abstractSpectral energy distributions are presented for 94 young stars surrounded by disks in the Serpens Molecular Cloud, based on photometry and Spitzer/IRS spectra. Most of the stars have spectroscopically determined spectral types. Taking a distance to the cloud of 415 pc rather than 259 pc, the distribution of ages is shifted to lower values, in the 1-3Myr range, with a tail up to 10 Myr. The mass distribution spans 0.2-1.2 M-circle dot, with median mass of 0.7 M-circle dot. The distribution of fractional disk luminosities in Serpens resembles that of the young Taurus Molecular Cloud, with most disks consistent with optically thick, passively irradiated disks in a variety of disk geometries (L-disk/L-star similar to 0.1). In contrast, the distributions for the older Upper Scorpius and. Chamaeleontis clusters are dominated by optically thin lower luminosity disks (L-disk/L-star similar to 0.02). This evolution in fractional disk luminosities is concurrent with that of disk fractions: with time disks become fainter and the disk fractions decrease. The actively accreting and non-accreting stars (based on H alpha data) in Serpens show very similar distributions in fractional disk luminosities, differing only in the brighter tail dominated by strongly accreting stars. In contrast with a sample of Herbig Ae/Be stars, the T Tauri stars in Serpens do not have a clear separation in fractional disk luminosities for different disk geometries: both flared and flat disks present wider, overlapping distributions. This result is consistent with previous suggestions of a faster evolution for disks around Herbig Ae/Be stars. Furthermore, the results for the mineralogy of the dust in the disk surface (grain sizes, temperatures and crystallinity fractions, as derived from Spitzer/IRS spectra) do not show any correlation to either stellar and disk characteristics or mean cluster age in the 1-10 Myr range probed here. A possible explanation for the lack of correlation is that the processes affecting the dust within disks have short timescales, happening repeatedly, making it difficult to distinguish long-lasting evolutionary effects.en_US
dc.description.sponsorshipNetherlands Organization for Scientific Research (NWO)en_US
dc.description.sponsorshipNetherlands Research School for Astronomy (NOVA)en_US
dc.description.sponsorshipNASAen_US
dc.description.sponsorshipNASA through JPL/Caltechen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectcircumstellar matteren_US
dc.subjectmethods: statisticalen_US
dc.subjectplanetary systemsen_US
dc.subjectprotoplanetary disksen_US
dc.subjectstars: pre-main sequenceen_US
dc.subjectspitzer c2d surveyen_US
dc.subjectt-tauri starsen_US
dc.subjectscorpius ob associationen_US
dc.subjectlow-massen_US
dc.subjectstarsen_US
dc.subjectspectral energy-distributionsen_US
dc.subjectyoung stellar objectsen_US
dc.subjectherbigen_US
dc.subjectae/be systemsen_US
dc.subjectx-ray-radiationen_US
dc.subjectcircumstellar disksen_US
dc.subjectmolecular clouden_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Physical Structure Of Protoplanetary Disks: The Serpens Cluster Compared With Other Regionsen_US
dc.typeArticleen_US
dc.description.departmentMcDonald Observatoryen_US
dc.identifier.Filename2013_01_serpenscluster.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/762/2/128en_US
dc.contributor.utaustinauthorOliveira, Isaen_US
dc.relation.ispartofserialAstrophysical Journalen_US


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