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dc.contributor.authorFernandes, Rachel B.
dc.contributor.authorLong, Zachary C.
dc.contributor.authorPikhartova, Monika
dc.contributor.authorSitko, Michael L.
dc.contributor.authorGrady, Carol A.
dc.contributor.authorRussell, Ray W.
dc.contributor.authorLuria, David M.
dc.contributor.authorTyler, Dakotah B.
dc.contributor.authorBayyari, Ammar
dc.contributor.authorDanchi, William
dc.contributor.authorWisniewski, John P.
dc.date.accessioned2018-05-01T22:46:17Z
dc.date.available2018-05-01T22:46:17Z
dc.date.issued2018-03-28
dc.identifier.citationRachel B. Fernandes et al 2018 ApJ 856 103en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aaaae7
dc.identifier.urihttp://hdl.handle.net/10150/627533
dc.description.abstractWe present five epochs of near-IR observations of the protoplanetary disk around MWC 480 (HD 31648) obtained with the SpeX spectrograph on NASA's Infrared Telescope Facility between 2007 and 2013, inclusive. Using the measured line fluxes in the Pa beta and Br gamma lines, we found the mass accretion rates to be (1.26-2.30) x 10(-7) M-circle dot yr(-1) and (1.4-2.01) x 10(-7) M-circle dot yr(-1), respectively, but which varied by more than 50% from epoch to epoch. The spectral energy distribution reveals a variability of about 30% between 1.5 and 10 mu m during this same period of time. We investigated the variability using of the continuum emission of the disk in using the Monte-Carlo Radiative Transfer Code HOCHUNK3D. We find that varying the height of the inner rim successfully produces a change in the NIR flux but lowers the far-IR emission to levels below all measured fluxes. Because the star exhibits bipolar flows, we utilized a structure that simulates an inner disk wind to model the variability in the near-IR, without producing flux levels in the far-IR that are inconsistent with existing data. For this object, variable near-IR emission due to such an outflow is more consistent with the data than changing the scale height of the inner rim of the disk.en_US
dc.description.sponsorshipNASA Exoplanet Research Program [NNX16AJ75G, NNX17AF88G]; NASA Origins of Solar Systems Funding [NNG16PX39P]; National Aeronautics and Space Administration; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA's Science Mission Directorateen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/856/i=2/a=103?key=crossref.01024da78286570cce286867df7e90aaen_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectplanet-disk interactionsen_US
dc.subjectprotoplanetary disksen_US
dc.subjectStars: individual (MWC 480)en_US
dc.subjectstars: variables: T Tauri, Herbig Ae/Been_US
dc.titleVariability of Disk Emission in Pre-main-sequence and Related Stars. IV. Investigating the Structural Changes in the Inner Disk Region of MWC 480en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume856
dc.source.issue2
dc.source.beginpage103
refterms.dateFOA2018-05-01T22:46:17Z


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