Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4407b&link_type=abstract
American Astronomical Society Meeting 208, #44.07; Bulletin of the American Astronomical Society, Vol. 38, p.119
Astronomy and Astrophysics
Astronomy
Scientific paper
Caby photometry has been used successfully to determine chemical compositions on a wide variety of stars, including main-sequence stars, red giants, and RR Lyrae variables. The success of Caby photometric studies of RR Lyr stars has initiated the application of this system to Cepheid variables. The sensitivity of the Caby photometric indices to metallicity decreases in stars of higher temperatures, and contamination from the Hɛ line makes use of the system undesirable in spectral class A and earlier. However, because sensitivity increases with the lower temperatures of the G and K regions, it might be expected that Caby photometry would be particularly useful for stars further up the Great Sequence of pulsational variables from Cepheids. RV Tauri stars are supergiant pulsational variables in the K, G, and occasionally F spectral classes. Few of these stars have had high-dispersion spectroscopic determinations of abundances, and abundance determinations from photometric surveys using, for example, DDO photometry, do not give consistent results. The physical peculiarities of RV Tau stars that have afflicted previous photometric studies are examined with respect to Caby photometry. The multiple layers present in the atmosphere at all phases should have less effect on Caby abundance determinations than the periods of intense veiling that occur in some stars particularly during rising light. Caby observations of bright RV Tau stars have been taken at Lowell Observatory and Behlen Observatory to ascertain whether this photometric system gives the same abundance at different phases in an RV Tau star’s pulsational cycle.
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