The pioneering studies of RR Lyrae stars in globular clusters by Oosterhoff and by Sawyer Hogg in the 1930s and 1940s called attention to interesting systematic differences among RR Lyrae populations in different systems. When such studies were extended to the dwarf spheroidal companions of the Milky Way in the 1960s, it was found that the average properties of their RR Lyrae stars were often different from those that had previously been observed in globular clusters. Observations of RR Lyrae stars have now extended to the Andromeda Galaxy and other Local Group systems, with still greater variety being apparent. Our understanding of the reasons for these differences among the RR Lyrae populations in different systems is by no means complete, but properties of RR Lyrae stars within these different systems are tied to differing horizontal branch morphologies and also shed light upon scenarios for the formation of the Galaxy.
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16 September 2009
STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference
31 May–5 June 2009
Santa Fe, New Mexico (USA)
Research Article|
September 16 2009
RR Lyrae Variables in Stellar Systems
Horace A. Smith;
Horace A. Smith
aDept. of Physics and Astronomy, Michigan State University, East Lansing, MI, USA 48824
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Márcio Catelan;
Márcio Catelan
bPontificia Universidad Catolica de Chile, Departamento de Astronomía y Astrofísica, Santiago, Chile
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Gisella Clementini
Gisella Clementini
cINAF Osservatorio Astronomico di Bologna, Via Ranzani n. 1, 40127 Bologna, Italy
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AIP Conf. Proc. 1170, 179–187 (2009)
Citation
Horace A. Smith, Márcio Catelan, Gisella Clementini; RR Lyrae Variables in Stellar Systems. AIP Conf. Proc. 16 September 2009; 1170 (1): 179–187. https://doi.org/10.1063/1.3246438
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