classical Cepheid

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'classical Cepheid' can also refer to...

classical Cepheid

classical Cepheid

Frequency analysis of Cepheids in the Large Magellanic Cloud: new types of classical Cepheid pulsators

Reddenings of FGK supergiants and classical Cepheids from spectroscopic data

The VMC survey - V. First results for classical Cepheids⋆

Period–colour and amplitude–colour relations in classical Cepheid variables – V. The Small Magellanic Cloud Cepheid models

Period–colour and amplitude–colour relations in classical Cepheid variables – III. The Large Magellanic Cloud Cepheid models

A lack of classical Cepheids in the inner part of the Galactic disc

Discovery of the spectroscopic binary nature of the classical Cepheids FN Aql and V1344 Aql

Empirical period–colour and amplitude–colour relations for Classical Cepheids and RR Lyrae variables

Predicted properties of galactic and magellanic classical Cepheids in the SDSS filters

Period–colour and amplitude–colour relations in classical Cepheid variables

Period–colour and amplitude–colour relations in classical Cepheid variables – IV. The multiphase relations

The occurrence of binary evolution pulsators in classical instability strip of RR Lyrae and Cepheid variables

The VMC survey – XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids

Physical parameters and the projection factor of the classical Cepheid in the binary system OGLE-LMC-CEP-0227

CORS Baade–Wesselink method in the Walraven photometric system: the period–radius and the period–luminosity relation of classical Cepheids

Mode identification of three low-amplitude classical Cepheids: V1334 Cyg, V440 Per and V636 Cas

The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids


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A Population I Cepheid variable, sometimes known as a Delta Cephei star; abbr. DCEP. In contrast to the superficially similar W Virginis stars of Population II, classical Cepheids are massive (5–15 solar masses), young bright giants or supergiants found exclusively in the disk population of galaxies, where they are often members of open clusters. The periods are 1–135 days, with amplitudes of 0.5–2 mag. The stars exhibit well-defined period–luminosity and period–luminosity–colour relations that are the basis of a widely used method of determining extragalactic distances.

Subjects: Astronomy and Astrophysics.

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