2001/04/18 by R. De Santis, R. de Santis · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2001.04618.x
published as Mon.Not.Roy.Astron.Soc. 326 (2001) 397 · 6 pages, 5 postscript figures, accepted for publication on MNRAS
arxiv created 2001/04/18 · openalex publication_date 2001/09/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In this paper, by assuming the equilibrium temperatures of RRab Lyrae variables defined by Carney, Storm & Jones as correct we show that temperatures derived from (B — V) colour (mean colour over the pulsational cycle calculated on the magnitude scale) transformations by Bessel, Castelli & Plez are consistent with the Carney et al. equilibrium temperatures within a probable error of δ log Te = ±0.003. As a consequence, it is shown that the pulsational temperature scale temperature—period—blue amplitude [Teff = ƒ(P,AB)] relation provided by De Santis, who studied the (B — V) colour of about 70 stars of Lub's sample, is a suitable relation, being reddening- and metallicity-free, to calculate equilibrium temperatures for RRab variables. This relation is independent of variable mass and luminosity within a large range of period-shift from the mean period—amplitude relation valid for Lub's sample of variables. On the contrary, it is also shown that a temperature—amplitude—metallicity relation is strictly dependent on the period—amplitude relation of the sample used for calibrating it: we prove that this means it is dependent on both the mass and luminosity variations of variables.