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Theoretical modeling of the RR Lyrae variables in NGC 1851

Journal
Date Issued
2015
Author(s)
Kunder, A.
•
Salaris, M.
•
•
de Propris, R.
•
Walker, A.
•
Stetson, P. B.
•
Catelan, M.
•
Amigo, P.
Abstract
The 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 (Ỹ0.248-0.270) 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 (Ỹ0.270-0.280) have longer periods at a given amplitude, as is seen with Oosterhoff II (OoII) RR Lyrae variables, whereas the RR Lyrae variables with Ỹ0.248-0.270 have shorter periods, exhibiting properties of Oosterhoff I (OoI) variables.
Volume
86
Start page
199
Uri
Url
Issn Identifier
0037-8720
Ads BibCode
2015MmSAI..86..199K
Rights
open.access
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