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- Title
The dynamical mass of a classical Cepheid variable star in an eclipsing binary system.
- Authors
Pietrzyński, G.; Thompson, I. B.; Gieren, W.; Graczyk, D.; Bono, G.; Udalski, A.; Soszyński, I.; Minniti, D.; Pilecki, B.
- Abstract
Stellar pulsation theory provides a means of determining the masses of pulsating classical Cepheid supergiants-it is the pulsation that causes their luminosity to vary. Such pulsational masses are found to be smaller than the masses derived from stellar evolution theory: this is the Cepheid mass discrepancy problem, for which a solution is missing. An independent, accurate dynamical mass determination for a classical Cepheid variable star (as opposed to type-II Cepheids, low-mass stars with a very different evolutionary history) in a binary system is needed in order to determine which is correct. The accuracy of previous efforts to establish a dynamical Cepheid mass from Galactic single-lined non-eclipsing binaries was typically about 15-30% (refs 6, 7), which is not good enough to resolve the mass discrepancy problem. In spite of many observational efforts, no firm detection of a classical Cepheid in an eclipsing double-lined binary has hitherto been reported. Here we report the discovery of a classical Cepheid in a well detached, double-lined eclipsing binary in the Large Magellanic Cloud. We determine the mass to a precision of 1% and show that it agrees with its pulsation mass, providing strong evidence that pulsation theory correctly and precisely predicts the masses of classical Cepheids.
- Subjects
STARS; BINARY stars; STELLAR oscillations; CEPHEIDS; COMPACT objects (Astronomy); ASTRONOMY; ECLIPSES; STELLAR structure
- Publication
Nature, 2010, Vol 468, Issue 7323, p542
- ISSN
0028-0836
- Publication type
Article
- DOI
10.1038/nature09598