The luminosity scale of RR Lyrae stars with the Baade-Wesselink method. II - The absolute magnitudes of 13 field RR Lyrae stars

Liu, Tianxing; Janes, K. A.

doi:10.1086/168688

Cited by 89 publications

(118 citation statements)

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“…In fact, the ultraviolet excess can be satisfactorily explained for the most part as due to the change in the effective surface gravity during the pulsation cycle. This has been pointed out by both McNamara and Feltz (1977) and Liu and Janes (1990).…”

Section: Discussionmentioning

confidence: 79%

“…A great deal has been written about the virtue of utilizing the (V-K) index to infer the temperatures required for the B-W analysis (Liu and Janes, 1990;Jones et al 1992;Carney et al 1992;Femley 1993). In brief, the (V-K) index yields a smoother temperature variation, the phases of maximum angular diameter and maximum radius match, (V-K) has a longer wavelength baseline, is less sensitive to metallicity and gravity variations, is less sensitive to shockwave effects near maximum fight, and gives a better overall fit of the angular diameters versus phase curves.…”

Section: Discussionmentioning

confidence: 99%

“…For some stars I have estimated the T tfi value from the {V-K) data given. In all cases the T eff value is determined from the older Kurucz models (see Liu and Janes 1990). In columns 11-14 we list the mean effective temperature, T{B-V), T{V-R C ), T(V-I C ), and T(b-y) inferred from the new Kurucz (1994) Femley (1993) points out that mean log g values of RR Lyrae variables lie in the range 2.75-2.95.…”

Section: Discussionmentioning

confidence: 99%

“…The turn-off luminosity of globular clusters in turn depends on determining accurate distance to the clusters; therefore, the age determination of the clusters depends on the luminosity of the RR Lyrae variables. Liu and Janes (1990) were the first to demonstrate convincingly what had long been suspected-that the luminosities of the RR Lyrae stars are a function of their metallicity. This obviously complicates the problem of employing these stars to find distances.…”

Section: Introductionmentioning

confidence: 90%

“…The spectroscopic angular diameter 2Rid can then be compared with the photometric angular diameter 6 calculated from equation (6), where d is the distance to the star in parsec. The distance to the star is found (Liu and Janes 1990) by minimizing the quantity: Table 1. The solid line is a least-square fit to the data plotted and corresponds to Eq.…”

Section: Absolute Magnitudes Of Rr Lyrae Variablesmentioning

confidence: 99%

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The Absolute Magnitudes of the RR Lyrae Stars

McNamara¹

1997

PASP

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ABSTRACT. We present a new calibration of the relationship between the absolute magnitudes and metal abundances, [Fe/H], of RR Lyrae stars. Temperatures inferred from optical and near-infrared color indices and the new Kurucz models are utilized in conjunction with Baade-Wesselink solutions to derive absolute magnitudes. Temperatures inferred from the optical and near-infrared photometry are -200-300 K higher for the variables than those given from (V-K) color indices and the older Kurucz models. We find M v = 0.287[Fe/H]+ 0.964. This equation gives higher luminosities ( -0.2 mag) for the metal-poor variables than previous B-W calibrations. The RR Lyrae stars in the Large Magellanic Cloud in conjunction with our calibration yield a distance modulus of 18.53. Thus, the Cepheids and RR Lyrae stars give identical distance moduli at ^0.1 mag level. The repercussions of the higher temperatures and higher luminosities of RR Lyrae stars on the distances and ages of globular clusters, distance to the galactic center, the Hubble constant and age of the Universe, and the masses of RR Lyrae stars are discussed.

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Section: Discussionmentioning

confidence: 79%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 90%

Section: Absolute Magnitudes Of Rr Lyrae Variablesmentioning

confidence: 99%

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