Updated pulsation models for anomalous Cepheids

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dc.creatorMarconi, M.
dc.creatorFiorentino, G.
dc.creatorCaputo, F.
dc.date2004-01-16
dc.date.accessioned2026-07-07T13:02:31Z
dc.date.available2026-07-07T13:02:31Z
dc.descriptionA theoretical investigation of the pulsation behavior of so-named ``anomalous'' Cepheids is presented. The study is based on nonlinear convective pulsation models with $Z$=0.0001 and 0.0004, mass in the range 1.3-2.2 Mo and various luminosity levels. Based on these computations, we derive period, bolometric light curves and the edges of the instability strip, showing that a variation of the metal abundance from Z=0.0001 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.
dc.description14 pages, 17 postscript figures, accepted for publication on A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/0401332
dc.identifierhttp://arxiv.org/abs/astro-ph/0401332
dc.identifierAstron.Astrophys.417:1101-1114,2004
dc.identifierdoi:10.1051/0004-6361:20040020
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/226477
dc.subjectAstrophysics
dc.titleUpdated pulsation models for anomalous Cepheids
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