Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21343313c&link_type=abstract
American Astronomical Society, AAS Meeting #213, #433.13; Bulletin of the American Astronomical Society, Vol. 41, p.303
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an analysis of the period-V-amplitude plane for RR0 Lyrae stars (fundamental mode pulsators) with "normal" light curves in the Bulge field stars from the MACHO Bulge fields. Although Bulge globular clusters have RR Lyraes that divide into two reasonably distinct groups according to the average period of the RR0 Lyraes (Oosterhoff 1939), there is no evidence of a gap between Oosterhoff I and II stars in the Bulge field star sample. A comparative study of stars with similar metallicities but different periods is carried out; here the Oosterhoff type is characterized by period shifts, or difference between the periods of RR Lyrae variables at fixed amplitude. The period shift analysis shows that RR0 variables with period shifts similar to Oosterhoff II clusters are about 0.2 mag brighter than RR0 variables with period shifts similar to Oosterhoff I clusters. Reliance upon a single Mv(RR)-[Fe/H] relation may be inappropriate when considering populations with different period shifts. This agrees with Clement & Shelton (1999) who concluded that the V Amplitude for a given period for RR0 stars is a function of evolutionary state and not just of metal abundance. We discuss the trends between metallicity and long and short period RR Lyrae stars as a function of distance from the plane.
Chaboyer Brian C.
Kunder Andrea
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