Other
Scientific paper
Aug 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248..161s&link_type=abstract
Astrophysical Journal, Part 1, vol. 248, Aug. 15, 1981, p. 161-176.
Other
193
Blue Stars, Giant Stars, Globular Clusters, Light Curve, Stellar Evolution, Stellar Oscillations, Variable Stars, Abundance, Line Spectra, Lyra Constellation, Stellar Magnitude, Stellar Mass, Stellar Models, Stellar Temperature
Scientific paper
Data for RR Lyrae stars in six clusters are used to test the conclusion of Paper I that, at every temperature, period shifts exist between variables in one cluster relative to those in another of a different Oosterhoff group. Variables in M3, M4, M15, NGC 6171, NGC 6891, and ωCen have the same shifts in the period-temperature as in the period-amplitude relations; no shifts occur in the temperature- amplitude relation.
The period residuals, Δ log P, determined for individual stars in M3 and in ω Cen, correlate with their observed apparent magnitudes; hence, the observed spread in LRR is real. Brighter variables than others in the same cluster have longer periods at fixed Te or A. The data are consistent with ΔMbol = 3Δ log P expected from P 1/2 = constant at fixed mass.
Combining the period deviations at fixed amplitude with the observed magnitude variations leads to a period-luminosity- amplitude relation for equal metallicity ab RR Lyrae variables of the form Mbol = Mbol(M315.52) -3(log P+0.l29AB +0.088), where Mbol(M3l5.52) is the absolute magnitude of RR Lyrae stars in M3 that have Mbol = 15.52. The coefficient of the period-amplitude term will be -4.2 rather than -3 if mass is a function of metallicity as predicted by the models.
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