Aims. We use parallax data from the Gaia second data release (GDR2), combined with
parallax data based on HIPPARCOS and HST data, to derive the period–luminosity …

Context. The universality of the Cepheid period-luminosity (PL) relations has been under
discussion since metallicity effects were assumed to play a role in the value of the intercept …

Context. The cross correlation method (hereafter CC) is widely used to derive the radial
velocity curve of Cepheids when the signal to noise ratio of the spectra is low. However, if it …

Context. The Baade-Wesselink (BW) method of distance determination of Cepheids is used
to calibrate the distance scale. Various versions of this method are mainly based on …

Polaris is the nearest and brightest classical Cepheid, and pulsates with a period of about 4
d. It has long been known as a single-lined spectroscopic binary with an orbital period of 30 …

Context. The parallax of pulsation, and its implementations such as the Baade-Wesselink
method and the infrared surface brightness technique, is an elegant method to determine …

The 30 yr orbit of the Cepheid Polaris has been followed with observations by the Center for
High Angular Resolution Astronomy (CHARA) Array from 2016 through 2021. An additional …

An analytical derivation is presented for computing mass-loss rates of Cepheids by using the
method of Castor, Abbott, and Klein modified to include a term for momentum input from …

Cepheid stars play a considerable role as extragalactic distances indicators, thanks to the
simple empirical relation between their pulsation period and their luminosity. They overlap …

Context. Estimating the metallicity of classical Cepheids is of prime importance for studying
metallicity effects on stellar evolution and the chemical evolution of galaxies, as well as on …