Improved Baade-Wesselink surface brightness relations
نویسندگان
چکیده
منابع مشابه
Improved Baade-Wesselink surface-brightness relations
Recent, and older accurate, data on (limb-darkened) angular diameters is compiled for 221 stars, as well as BV RIJK[12][25] magnitudes for those objects, when available. Nine stars (all M-giants or supergiants) showing excess in the [12− 25] colour are excluded in the analysis as this may indicate the present of dust influencing the optical and near-infrared colours as well. Based on this large...
متن کاملOn the Inversion of the Baade-wesselink Technique
A general framework is given for the inversion of a "two-point" formulation of the Baade-Wesselink technique. This means that phases of equal radius are selected and used to get information regarding brightness and temperature. The inversion method is used to evaluate the surface brightness/(V -R) relation in two classical Cepheids, V482 Sco and R TrA. The slope found is consistent with previou...
متن کاملBaade-Wesselink distances and the effect of metallicity in classical cepheids
Context. The metallicity dependence of the Cepheid PL-relation is of importance in establishing the extra-galactic distance scale. Aims. The aim of this paper is to investigate the metallicity dependence of the PL-relation in V and K based on a sample of 68 Galactic Cepheids with individual Baade-Wesselink distances (some of the stars also have an HST-based parallax) and individually determined...
متن کاملConsistent distances from Baade-Wesselink analyses of Cepheids and RR Lyraes
By using the same algorithm in the Baade-Wesselink analyses of Galactic RR Lyrae and Cepheid variables, it is shown that, within 0.03 mag 1σ statistical error, they yield the same distance modulus for the Large Magellanic Cloud. By fixing the zero point of the color–temperature calibration to those of the current infrared flux methods and using updated period–luminosity–color relations, we get ...
متن کاملCepheid distances from Interferometry
Long baseline interferometry is now able to resolve the pulsational change of the angular diameter of a significant number of Cepheids in the solar neighborhood. This allows the application of a new version of the Baade-Wesselink (BW) method to measure their distance, for which we do not need to estimate the star’s temperature. Using angular diameter measurements from the VLT Interferometer, we...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2004
ISSN: 0035-8711,1365-2966
DOI: 10.1111/j.1365-2966.2004.08121.x