Theoretical modeling of the RR Lyrae variables in NGC 1851

Simple item page
dc.catalogadorpau
dc.contributor.authorKunder, A.
dc.contributor.authorSalaris, M.
dc.contributor.authorCassisi, S.
dc.contributor.authorde Propris, R.
dc.contributor.authorWalker, A.
dc.contributor.authorStetson, P. B.
dc.contributor.authorCatelan, Marcio
dc.contributor.authorAmigo, P.
dc.date.accessioned2024-03-05T15:14:35Z
dc.date.available2024-03-05T15:14:35Z
dc.date.issued2015
dc.description.abstractThe RR Lyrae instability strip (IS) in NGC 1851 is investigated, and a model is presented which reproduces the pulsational properties of the RR Lyrae population. In our model, a stellar component within the IS that displays minor helium variations (Y∼0.248-0.270) is able to reproduce the observed periods and amplitudes of the RR Lyrae variables, as well as the frequency of fundamental and first-overtone RR Lyrae variables. The RR Lyrae variables therefore may belong to an He-enriched second generation of stars. The RR Lyrae variables with a slightly enhanced helium (Y∼0.270-0.280) have longer periods at a given amplitude, as is seen with Oosterhoff II (OoII) RR Lyrae variables, whereas the RR Lyrae variables with Y∼0.248-0.270 have shorter periods, exhibiting properties of Oosterhoff I (OoI) variables. %.
dc.fuente.origenORCID
dc.identifier.doi10.48550/arXiv.1301.2575
dc.identifier.urihttps://doi.org/10.48550/arXiv.1301.2575
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/83974
dc.information.autorucInstituto de Astrofísica; Catelan , Marcio; 0000-0001-6003-8877; 1001556
dc.language.isoen
dc.rightsacceso abierto
dc.titleTheoretical modeling of the RR Lyrae variables in NGC 1851
dc.typeartículo
sipa.codpersvinculados1001556
sipa.trazabilidadORCID;2024-01-22
Files
Collections
Artículos de revistas