Analysis of a detached eclipsing binary at near the turnoff point of the open cluster NGC 6791 in Kepler field |
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| Institution: | 1. Department of Astronomy & Space Sciences, Faculty of Science, Ege University, 35100 Bornova, ?zmir, Turkey;2. Department of Physics, University of Zagreb, Bijenicka cesta 32, 10000 Zagreb, Croatia;3. Department of Astronomy & Space Sciences, Erciyes University, Kayseri, Turkey;4. Department of Astronomy & Space Sciences, Graduate School of Science and Engineering, Istanbul University, 34116, Beyazt, Istanbul, Turkey;1. ICFAI University Tripura, Kamalghat, Tripura Mohanpur-799210, India;2. Department of Mathematics, BITS Pilani K K Birla, Goa Campus, Goa 403726, India;1. Physics Department, University of Rijeka, Radmile Matej?i?, 51000 Rijeka, Croatia;2. INAF Astronomical Observatory of Padova, via dell’Osservatorio 8, Asiago (VI) 36012, Italy;1. Department of Mathematics, Faculty of Science, Taibah University, Madina 344, Saudi Arabia;2. Department of Astronomy, Faculty of Science, Cairo University, Cairo 12613, Egypt;1. Department of Physics, Hamedan Branch, Islamic Azad University, Hamedan, Iran;2. Department of Science, Hamedan University of Technology, Hamedan 65155, Iran;3. Department of Mathematics, Hamedan Branch, Islamic Azad University, Hamedan, Iran |
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| Abstract: | We analyzed high-precision Kepler photometry and high–resolution UVES and GIRAFFE spectroscopy from ESO Science Archieve for a double–lined eclipsing binary star in the field of the high metallicity old open cluster NGC 6791. Earlier measurements of the masses and radii of the detached system were not accurate enough for photometric and spectroscopic data to demonstrate that there are significant differences between current stellar models. Here we improved on the result and add follow-up measurements of the system. Data from the Kepler archive makes it clear that the system has an inclination that is close to 90°. The combination of radial velocity and Kepler light curve of the system were analysed simultaneously, which allows us to determine a reliable mass for the primary and secondary star and radii for both stars, and to constrain the cluster age. The characteristics of the primary star at the cluster turnoff indicate an age of 8.5 ± 0.12 Gyr, consistent with earlier analysis of the color–magnitude diagram. The brighter star in the binary also produces a precision estimate of the distance modulus, independent of reddening estimates: (m-M)V (mag)=13.899 ± 0.117. The secondary star is not expected to have evolved significantly, but its radius is more than 10% larger than predicted by models. The hallmark is useful for testing the idea that radius inflation can occur in short period binaries for stars with significant convective envelopes due to the inhibition of energy transport by magnetic fields. |
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