2004/01/16 by M. Marconi, G. Fiorentino, F. Caputo · 1 citation
Physics and Astronomy · #Absolute magnitude #Amplitude #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Cepheid variable #Galaxies: Formation, Evolution, Phenomena #Galaxy #Instability #Instability strip #Light curve #Luminosity #Magnitude (astronomy) #Optics #Overtone #Physics #Spectral line #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20040020
published as Astron.Astrophys.417:1101-1114,2004 · 14 pages, 17 postscript figures, accepted for publication on A&A
arxiv created 2004/01/16 · openalex publication_date 2004/03/26 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A theoretical investigation of the pulsation behavior of so-named “anomalous” Cepheids is presented. The study is based on nonlinear convective pulsation models with and 0.0004, mass in the range 1.3-2.2 and various luminosity levels. Based on these computations, we derive periods, bolometric light curves and the edges of the instability strip, showing that a variation of the metal abundance from to 0.0004 has quite small effects on these quantities. Then, using bolometric corrections and color-temperature transformations, we are able to provide the predicted relations connecting pulsational properties (periods, amplitudes) with magnitudes and colors in the various photometric bands. The theoretical pulsational scenario is compared to observed anomalous Cepheids in dwarf spheroidal galaxies and, in particular, the predicted mass-dependent Period-Magnitude-Amplitude and Period-Magnitude-Color relations are used to estimate individual mass values, as well as to discriminate between fundamental (F) and first-overtone (FO) pulsators.