An Oosterhoff Analysis of the Galactic Bulge Field RR Lyrae stars: Implications On Their Absolute Magnitudes

Details An Oosterhoff Analysis of the Galactic Bulge Field RR Lyrae stars: Implications On Their Absolute Magnitudes An Oosterhoff Analysis of the Galactic Bulge Field RR Lyrae stars: Implications On Their Absolute Magnitudes

Publishing date

Sep 2009

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1170..188k&link_type=abstract

Journals

STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP Conference Proceedin

Science

Other

Additional info 3

Neutrino, Muon, Pion, And Other Elementary Particles, Cosmic Rays, Cepheids, Quasars, Active Or Peculiar Galaxies, Objects, And Systems

Type

Scientific paper

Abstract

The period-V-amplitude plane for fundamental mode pulsator RR Lyrae stars in the MACHO Bulge fields is examined. Only stars with ``normal'' light curves are used in the analysis. Although the RR Lyraes in Bulge globular clusters divide into two distinct groups based on the average periods [12], no gap between Oosterhoff I and II stars in the Bulge field star sample is seen. The main Δ log P distribution of the Bulge RR0 Lyrae field star population is shifted by about 0.02 days with regard to the Milky Way Oosterhoff I population. Stars with Δ log P>0.06 days are seen in the sample, a rare property of RR Lyrae in Milky Way globular clusters. A comparative study of the Bulge field stars with similar metallicities but different Oosterhoff types is carried out, and it is shown that Bulge field RR0 Lyrae variables with OoII-like Δ log P values are about 0.2 mag brighter than RR0 Lyrae variables with OoI-like Δ log P value. Hence, an RR Lyrae MVRR-[Fe/H] relation may be inaccurate when considering populations with different Δ log P.

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