The faint Cepheids of the Small Magellanic Cloud: An evolutionary selection effect?

@article{Cordier2003TheFC,
  title={The faint Cepheids of the Small Magellanic Cloud: An evolutionary selection effect?},
  author={Daniel Cordier and M-J. Goupil and Yveline Lebreton},
  journal={Astronomy and Astrophysics},
  year={2003},
  volume={409},
  pages={491-501}
}
´ eaulieu, F-35700 Rennes, France.Received ; acceptedAbstract. Two problems about the faintest Small Magellanic Cloud (SMC) Cepheids are addressed. On one handevolutionary tracks fail to cross the Cepheid Instability Strip for the highest magnitudes (i.e. I-mag∼ 17) whereCepheids are observed; Mass-Luminosity relations (ML) obtained from evolutionary tracks disagree with Mass-Luminosity relations derived from observations. We find that the above failures concern models built with standardinput… 

Figures and Tables from this paper

Bright metal-poor variables: Why “Anomalous” Cepheids?
We investigate the theoretical scenario concerning the large sample of variables recently discovered in the dwarf, metal-poor irregular galaxy Leo A, focusing the attention on the “Anomalous” Cepheid
The beat Cepheids in the Magellanic Clouds: an analysis from the EROS-2 database
Context: A number of microlensing dark-matter surveys have produced tens of millions of light curves of individual background stars. These data provide an unprecedented opportunity for systematic
On the Cepheid Metallicity Dichotomy
With the aid of stellar atmosphere models, we derive iron abundances [Fe/H] from the OGLE B, V, I photometry on the Magellanic Cloud Cepheids. We show that in both clouds the average metallicities of
Synthetic properties of bright metal-poor variables I. "Anomalous" Cepheids
We present new grids of evolutionary models for the so-called "Anomalous" Cepheids (ACs), adopting Z = 0.0001 and various assumptions on the progenitor mass and mass-loss efficiency. These
Magellanic Cloud Cepheids: Pulsational and evolutionary modelling vs. observations
The pulsational properties of the Cepheid models along the evolutionary tracks from the Padova group (Girardi et al.), as calculated with our turbulent convective pulsation code, are in good
Disk of the Small Magellanic Cloud as traced by Cepheids
The structure and evolution of the disk of the Small Magellanic Cloud (SMC) are traced by studying the Cepheids. We aim to estimate the orientation measurements of the disk, such as the inclination
Synthetic properties of bright metal-poor variables
We present new grids of evolutionary models for the so-called “Anomalous” Cepheids (ACs), adopting Z = 0.0001 and various assumptions on the progenitor mass and mass-loss efficiency. These
Galactic cepheids. I. Elemental abundances and their implementation for stellar and galactic evolution
We have added data for 16 distant Cepheids observed with the echelle spectrograph of the Apache Point 3.5 m telescope to improve the correlations of abundance parameters with pulsation period and
Galactic Cepheids. II. Lithium
We report on the discovery of two lithium Cepheids in the Galaxy, based on observations made with the echelle spectrograph of the Apache Point Observatory. We have used high-resolution, high
Period–colour and amplitude–colour relations in classical Cepheid variables – II. The Galactic Cepheid models
In this paper, we construct full amplitude non-linear hydrodynamical models of fundamental mode Galactic Cepheids and analyse the resulting theoretical period-colour (PC) and amplitude-colour (AC)
...
1
2
...

References

SHOWING 1-10 OF 38 REFERENCES
Cepheid mass-luminosity relations from the Magellanic Clouds
The OGLE data base is used in conjunction with Kurucz atmosphere models to generate sets of period, eective temperature and luminosity for fundamental and overtone Magellanic Cloud Cepheids. The
Cepheid models based on self-consistent stellar evolution and pulsation calculations: The right answer?
We have computed stellar evolutionary models for stars in a mass range characteristic of Cepheid variables (3<m/M<12) for different metallicities representative of the Galaxy and the Magellanic
Magellanic Cloud Cepheids: Abundances
We have determined parameters and abundances for three SMC and nine LMC Cepheids that have not been previously studied spectroscopically for metallicity, as well as three SMC and one LMC Cepheids
Large Magellanic Cloud Bump Cepheids: Probing the Stellar Mass-Luminosity Relation
We present the results of nonlinear pulsation modeling of 20 bump Cepheids in the LMC. By obtaining an optimal fit to the observed V, R MACHO light curves, we have placed tight constraints on stellar
Improving the Mass Determination of Galactic Cepheids
We have selected a sample of Galactic Cepheids for which accurate estimates of radii, distances, and photometric parameters are available. The comparison between their pulsation masses, based on new
Ages and Metallicities of Five Intermediate-Age Star Clusters Projected Towards the Small Magellanic Cloud
Colour–magnitude diagrams are presented for the first time for L32, L38, K28 (L43), K44 (L68) and L116, which are clusters projected on to the outer parts of the Small Magellanic Cloud (SMC). The
A “Short” Distance to the Large Magellanic Cloud With the Hipparcos Calibrated Red Clump Stars
Following an approach developed by Paczynski & Stanek, we derive a distance to the Large Magellanic Cloud (LMC) by comparing red clump stars from the Hipparcos catalog with the red clump stars
Ten eclipsing binaries in the Small Magellanic Cloud: fundamental parameters and SMC distance
We present the first results of an observational programme to measure the fundamental parameters of over 100 eclipsing binaries in the Small Magellanic Cloud (SMC). The spectroscopic data were
THE PRIMORDIAL HELIUM ABUNDANCE: SYSTEMATIC EFFECTS AND A NEW DETERMINATION
We present new high-quality spectrophotometric observations of 27 supergiant H II regions in 23 low-metallicity blue compact galaxies (BCGs) with oxygen abundance 12 + log (O/H) between 7.22 and 8.17
The HST Key Project on the Extragalactic Distance Scale. XXVIII. Combining the Constraints on the Hubble Constant
Since the launch of the Hubble Space Telescope nine years ago, Cepheid distances to 25 galaxies have been determined for the purpose of calibrating secondary distance indicators. A variety of these
...
1
2
3
4
...