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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60406
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dc.creatorCaeley V. Pittmanpt_BR
dc.creatorPéter Ábrahámpt_BR
dc.creatorJuan M. Alcalápt_BR
dc.creatorSilvia Helena Paixao Alencarpt_BR
dc.creatorNicole Arulananthampt_BR
dc.creatorSylvie Cabritpt_BR
dc.creatorJochen Eislöffelpt_BR
dc.creatorEleonora Fiorellinopt_BR
dc.creatorKevin Francept_BR
dc.creatorManuele Gangipt_BR
dc.creatorKonstantin Grankinpt_BR
dc.creatorCatherine C. Espaillatpt_BR
dc.creatorGregory J. Herczegpt_BR
dc.creatorÁgnes Kóspálpt_BR
dc.creatorIgnacio Mendigutíapt_BR
dc.creatorJavier Sernapt_BR
dc.creatorLaura Venutipt_BR
dc.creatorConnor E. Robinsonpt_BR
dc.creatorThanawuth Thanathibodeept_BR
dc.creatorNuria Calvetpt_BR
dc.creatorJohn Wendebornpt_BR
dc.creatorJesus Hernándezpt_BR
dc.creatorCarlo F. Manarapt_BR
dc.creatorFred Walterpt_BR
dc.date.accessioned2023-10-31T21:40:49Z-
dc.date.available2023-10-31T21:40:49Z-
dc.date.issued2022-11-
dc.citation.volume164pt_BR
dc.citation.issue5pt_BR
dc.citation.spage1pt_BR
dc.citation.epage16pt_BR
dc.identifier.doihttps://doi.org/10.3847/1538-3881/ac898dpt_BR
dc.identifier.issn1538-3881pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60406-
dc.description.resumoThe coevolution of T Tauri stars and their surrounding protoplanetary disks dictates the timescales of planet formation. In this paper, we present magnetospheric accretion and inner disk wall model fits to near-UV (NUV) to near-IR (NIR) spectra of nine classical T Tauri stars in Orion OB1b as part of the Outflows and Disks around Young Stars: Synergies for the Exploration of ULLYSES Spectra (ODYSSEUS) survey. Using NUV–optical spectra from the Hubble UV Legacy Library of Young Stars as Essential Standards (ULLYSES) Director's Discretionary Program and optical–NIR spectra from the PENELLOPE VLT Large Programme, we find that the accretion rates of these targets are relatively high for the region's intermediate age of 5.0 Myr; rates are in the range of (0.5–17.2) × 10−8 M☉ yr−1, with a median value of 1.2 × 10−8 M☉ yr−1. The NIR excesses can be fit with 1200–1800 K inner disk walls located at 0.05–0.10 au from the host stars. We discuss the significance of the choice in extinction law, as the measured accretion rate depends strongly on the adopted extinction value. This analysis will be extended to the complete sample of T Tauri stars being observed through ULLYSES to characterize accretion and inner disks in star-forming regions of different ages and stellar populations.pt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofThe Astronomical Journalpt_BR
dc.rightsAcesso Abertopt_BR
dc.subjectPre-main sequence starspt_BR
dc.subjectStellar accretionpt_BR
dc.subjectStellar accretion diskspt_BR
dc.subjectProtoplanetary diskspt_BR
dc.subjectReddening lawpt_BR
dc.subjectInterstellar extinctionpt_BR
dc.subjectHubble Space Telescopept_BR
dc.subjectVery Large Telescopept_BR
dc.subject.otherAstronomiapt_BR
dc.subject.otherEstrelas - Formaçãopt_BR
dc.titleTowards a comprehensive view of accretion, inner disks, and extinction in classical T Tauri stars: an ODYSSEUS study of the Orion OB1b Associationpt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://iopscience.iop.org/article/10.3847/1538-3881/ac898dpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5171-8376pt_BR
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