Add to ORKGIt is shown that the oscillations of brightness in classical Cepheids and other 'pulsating' variable stars are caused rather by the passing of radial solitary waves through the photosphere of a star, than by pulsations of a star. Radial solitary waves also determine the oscillations of brightness in some other types of periodic variable stars ordinary not considered as pulsating stars
Context. Emission lines observed in radially pulsating stars are thought to be produced by atoms de-...
Space photometric data of the Kepler Cepheid, V1154 Cygni, and those of SZ Tauri (MOST photometry) i...
We analyse photometry of similar to 2000 Galactic Cepheids available in the OGLE Collection of Varia...
On the basis of observational data it is argued that RV Tauri variables, and probably yellow semireg...
In the first part of this paper, traditional methods of studying Cepheids are summarized, mentioning...
Classical Cepheids and RR Lyrae are very important primary distance indicators and stellar populatio...
Several closely related classes of variable stars—here called Cepheid variables—have long been known...
Several closely related classes of variable stars—here called Cepheid variables—have long been known...
Double mode pulsation is a very pervasive phenomenon in stars all over the Hertzsprung-Russell diagr...
As children we used to sing in wonderment of the twinkling stars above and many of us asked, “Why do...
Recent analyses of photometric data on globular clusters and galaxies enabled us to study more close...
We review techniques for measuring stellar oscillations in solar-type stars. Despite great efforts, ...
none39siWe discuss evolutionary and pulsation properties of classical Cepheids and RR Lyrae stars. W...
Various types of pulsating stars show periodic amplitude changes. The Fourier spectra of these stars...
Fourier decompositions have been made of the light curves of a large sample of RR Lyrae field stars....
Context. Emission lines observed in radially pulsating stars are thought to be produced by atoms de-...
Space photometric data of the Kepler Cepheid, V1154 Cygni, and those of SZ Tauri (MOST photometry) i...
We analyse photometry of similar to 2000 Galactic Cepheids available in the OGLE Collection of Varia...
On the basis of observational data it is argued that RV Tauri variables, and probably yellow semireg...
In the first part of this paper, traditional methods of studying Cepheids are summarized, mentioning...
Classical Cepheids and RR Lyrae are very important primary distance indicators and stellar populatio...
Several closely related classes of variable stars—here called Cepheid variables—have long been known...
Several closely related classes of variable stars—here called Cepheid variables—have long been known...
Double mode pulsation is a very pervasive phenomenon in stars all over the Hertzsprung-Russell diagr...
As children we used to sing in wonderment of the twinkling stars above and many of us asked, “Why do...
Recent analyses of photometric data on globular clusters and galaxies enabled us to study more close...
We review techniques for measuring stellar oscillations in solar-type stars. Despite great efforts, ...
none39siWe discuss evolutionary and pulsation properties of classical Cepheids and RR Lyrae stars. W...
Various types of pulsating stars show periodic amplitude changes. The Fourier spectra of these stars...
Fourier decompositions have been made of the light curves of a large sample of RR Lyrae field stars....
Context. Emission lines observed in radially pulsating stars are thought to be produced by atoms de-...
Space photometric data of the Kepler Cepheid, V1154 Cygni, and those of SZ Tauri (MOST photometry) i...
We analyse photometry of similar to 2000 Galactic Cepheids available in the OGLE Collection of Varia...