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dc.contributor.authorHarmanec P.
dc.contributor.authorKoubský P.
dc.contributor.authorNemravová J. A.
dc.contributor.authorRoyer F.
dc.contributor.authorBriot D.
dc.contributor.authorNorth P.
dc.contributor.authorLampens P.
dc.contributor.authorFrémat Y.
dc.contributor.authorYang S.
dc.contributor.authorBožić H.
dc.contributor.authorKotková L.
dc.contributor.authorŠkoda P.
dc.contributor.authorŠlechta M.
dc.contributor.authorKorčáková D.
dc.contributor.authorWolf M.
dc.contributor.authorZasche P.
dc.date1/2015
dc.date.accessioned2016-04-13T10:08:13Z
dc.date.available2016-04-13T10:08:13Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/3952
dc.descriptionhttp://esoads.eso.org/abs/2015A%26A...573A.107H
dc.languageeng
dc.rightsRestricted Access
dc.titleProperties and nature of Be stars. 30. Reliable physical properties of a semi-detached B9.5e+G8III binary BR CMi = HD 61273 compared to those of other well studied semi-detached emission-line binaries
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.source.titleAstronomy and Astrophysics
dc.source.volume573
dc.source.pageA107
Orfeo.peerreviewedYes
dc.identifier.doi10.1051/0004-6361/201424640
dc.identifier.urlhttp://esoads.eso.org/abs/2015A%26A...573A.107H
dc.source.editorEDP Sciences


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