Metal-poor type II cepheids with periods less than three days

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dc.contributor.authorKovtyukh V.
dc.contributor.authorWallerstein G.
dc.contributor.authorYegorova I.
dc.contributor.authorAndrievsky S.
dc.contributor.authorKorotin S.
dc.contributor.authorSaviane I.
dc.contributor.authorBelik S.
dc.contributor.authorDavis C.E.
dc.contributor.authorFarrell E.M.
dc.date.accessioned2022-08-17T21:24:30Z
dc.date.available2022-08-17T21:24:30Z
dc.date.issued2018-05
dc.descriptionIndexación Scopuses
dc.description.abstractWe have analyzed 10 high-resolution spectra of Type II Cepheids with periods less than 3 days. We find that they clearly separate into two groups: those with near or slightly below solar metallicities, and those with [Fe/H] between −1.5 and −2.0. While the former are usually called BLHer stars, we suggest that the latter be called UYEri stars. The UYEri subclass appears to be similar to the short period variables in globular clusters of the Galactic Halo. Globular clusters with [Fe/H] > −1.0 almost never have Type II Cepheids. © 2018. The Astronomical Society of the Pacific. All rights reserved.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.1088/1538-3873/aaacf7
dc.identifier.citationPublications of the Astronomical Society of the Pacific Volume 130, Issue 987May 2018 Article number 054201es
dc.identifier.doi10.1088/1538-3873/aaacf7
dc.identifier.issn00046280
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23563
dc.language.isoenes
dc.publisherInstitute of Physics Publishinges
dc.subjectPeriodes
dc.subjectMagellanic Cloudses
dc.subjectGlobular Clusterses
dc.subjectGlobular clusters: generales
dc.subjectStars: abundances, variable: cepheidses
dc.titleMetal-poor type II cepheids with periods less than three dayses
dc.typeArtículoes
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