Pulsating Hot Subdwarfs in Omega Centauri

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dc.catalogadormas
dc.contributor.authorRandall, S. K.
dc.contributor.authorCalamida, A.
dc.contributor.authorFontaine, G.
dc.contributor.authorMonelli, M.
dc.contributor.authorBono, G.
dc.contributor.authorAlonso, M. L.
dc.contributor.authorVan Grootel, V.
dc.contributor.authorBrassard, P.
dc.contributor.authorChayer, P.
dc.contributor.authorCatelan , Marcio
dc.contributor.authorLittlefair, S.
dc.contributor.authorDhillon, V. S.
dc.contributor.authorMarsh, T. R.
dc.date.accessioned2024-02-02T13:58:45Z
dc.date.available2024-02-02T13:58:45Z
dc.date.issued2016
dc.description.abstractWe recently discovered the first globular cluster hot subdwarf pulsators in Omega Centauri (ω Cen). These stars were initially thought to belong to the class of rapidly pulsating subdwarf B stars, which are well established among the field star population and have become showcases for asteroseismology. However, our spectroscopic analysis revealed the ω Cen variables to be significantly hotter than expected, indicating that they form a new class of subdwarf O pulsators clustered around 50 000 K, not known among the field star population. Non-adiabatic pulsation modelling suggests that the driver for the pulsations occurs via the same iron opacity mechanism that is at work in the rapidly pulsating subdwarf B stars....
dc.fuente.origenORCID
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/81272
dc.information.autorucInstituto de Astrofísica; Catelan , Marcio; 0000-0001-6003-8877; 1001556
dc.language.isoen
dc.rightsacceso abierto
dc.titlePulsating Hot Subdwarfs in Omega Centauri
dc.typeartículo
sipa.codpersvinculados1001556
sipa.trazabilidadORCID;2024-01-22
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