Infrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds

dc.contributor.authorKeller, Stefan
dc.date.accessioned2015-12-13T23:40:25Z
dc.date.available2015-12-13T23:40:25Z
dc.date.issued1999
dc.date.updated2015-12-12T09:29:02Z
dc.description.abstractWe present broadband infrared photometry for 52 late-type supergiants in the young Magellanic Cloud clusters NGC 330, 1818, 2004, and 2100. Standard models are seen to differ in the temperature they predict for the red supergiant population by on the order of 300 K. It appears that these differences are most probably due to the calibration of the mixing-length parameter αP in the outermost layers of the stellar envelope. Because αP apparently depends on the model used, we do not quantitatively compare αP between models. Qualitatively, we find that αP decreases with increased stellar mass within standard models. We do not find evidence that αP depends on metallicity.
dc.identifier.issn0004-6256
dc.identifier.urihttp://hdl.handle.net/1885/94455
dc.publisherUniversity of Chicago Press
dc.sourceAstronomical Journal
dc.subjectKeywords: Infrared radiation; Magellanic Clouds; Stars: late-type
dc.titleInfrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds
dc.typeJournal article
local.bibliographicCitation.lastpage894
local.bibliographicCitation.startpage889
local.contributor.affiliationKeller, Stefan, College of Physical and Mathematical Sciences, ANU
local.contributor.authoremailrepository.admin@anu.edu.au
local.contributor.authoruidKeller, Stefan, u9702857
local.description.notesImported from ARIES
local.description.refereedYes
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationMigratedxPub24050
local.identifier.citationvolume118
local.identifier.scopusID2-s2.0-0012453950
local.identifier.uidSubmittedByMigrated
local.type.statusPublished Version

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