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dc.contributor.authorDong, Ruobing
dc.contributor.authorNajita, Joan R.
dc.contributor.authorBrittain, Sean
dc.date.accessioned2018-12-05T20:49:43Z
dc.date.available2018-12-05T20:49:43Z
dc.date.issued2018-08-01
dc.identifier.citationRuobing Dong et al 2018 ApJ 862 103en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aaccfc
dc.identifier.urihttp://hdl.handle.net/10150/631109
dc.description.abstractSpiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of well-studied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 M-circle dot). Here we explore the origin of spiral arms in Herbig systems by studying their occurrence rates, disk properties, and stellar accretion rates. We find that two-arm spirals are more common in disks surrounding Herbig intermediate-mass stars than are directly imaged giant planet companions to mature A and B stars. If two-arm spirals are produced by such giant planets, this discrepancy suggests that giant planets are much fainter than predicted by hot-start models. In addition, the high stellar accretion rates of Herbig stars, if sustained over a reasonable fraction of their lifetimes, suggest that disk masses are much larger than inferred from their submillimeter continuum emission. As a result, gravitational instability is a possible explanation for multiarm spirals. Future observations can lend insights into the issues raised here.en_US
dc.description.sponsorshipNASA [NXX15AD94G, NNX16AJ81G, NNX15AD94G]; NSF-AST [1517014]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/862/i=2/a=103?key=crossref.7005c9af78e5767ffccd643c07b21720en_US
dc.rights© 2018. The American Astronomical Society.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectplanet-disk interactionsen_US
dc.subjectplanets and satellites: formationen_US
dc.subjectprotoplanetary disksen_US
dc.subjectstars: pre-main sequenceen_US
dc.subjectstars: variables: T Tauri, Herbig Ae/Been_US
dc.titleSpiral Arms in Disks: Planets or Gravitational Instability?en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_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.volume862
dc.source.issue2
dc.source.beginpage103
refterms.dateFOA2018-12-05T20:49:43Z


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