| Issue |
EPJ Web Conf.
Volume 152, 2017
Wide-Field Variability Surveys: A 21st Century Perspective – 22nd Los Alamos Stellar Pulsation – Conference Series Meeting
|
|
|---|---|---|
| Article Number | 07007 | |
| Number of page(s) | 8 | |
| Section | The distance scale in the era of large surveys | |
| DOI | https://doi.org/10.1051/epjconf/201715207007 | |
| Published online | 08 September 2017 | |
https://doi.org/10.1051/epjconf/201715207007
Araucaria Project: Pulsating stars in binary systems and as distance indicators
1 Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland
2 Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
3 Millennium Institute of Astrophysics, Santiago, Chile
* pilecki@camk.edu.pl
** wgieren@astro-udec.cl
Published online: 8 September 2017
Pulsating stars, like Cepheids or RR Lyrae stars, are ones of the most important distance indicators. They are also key objects for testing the predictions of stellar evolution and stellar pulsation theory. In the Araucaria Project we have studied these objects since 2002, measuring distances to the galaxies in the Local Group and beyond.
In 2010 we have for the first time confirmed spectroscopically the existence of a classical Cepheid in an eclipsing binary system. This has opened an opportunity to study in great details and with high accuracy (better than 1%) the physical parameters of these very important objects. First dynamical mass determination (Mcep = 4.16 ± 0.03 M⊙) let us solve the long-standing mass discrepancy problem. Since then we have measured masses for 6 classical Cepheids in binary systems and determined projection factors for three of them. One of the analyzed systems was confirmed to consist of two first-overtone Cepheids.
Type II Cepheids are recently becoming more important as distance indicators and astrophysics laboratory, although our knowledge of these stars is quite limited. Their evolutionary status is also not well understood and observational constraints are needed to confirm the current theories. We are presenting here our first results of the spectroscopic analysis of 4 of these systems. The masses of type II Cepheids seem consistent with the expected 0.5 − 0.6 M⊙. We also present first results of the fully modeled pulsator originally classified as peculiar W Vir star. The mass of this star is 1.51 ± 0.09 M⊙ and the p-factor 1.3 ± 0.03. It was eventually found not to belong to any typical Cepheid group.
© The Authors, published by EDP Sciences, 2017
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