Absolute dimensions of the low-mass eclipsing binary system NSVS 10653195
Astronomy and Astrophysics, ISSN: 1432-0746, Vol: 627
2019
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Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
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Article Description
Context. Low-mass stars in eclipsing binary systems show radii larger and effective temperatures lower than theoretical stellar models predict for isolated stars with the same masses. Eclipsing binaries with low-mass components are hard to find due to their low luminosity. As a consequence, the analysis of the known low-mass eclipsing systems is key to understand this behavior. Aims. We aim to investigate the mass-radius relation for low-mass stars and the cause of the deviation of the observed radii in low-mass detached eclipsing binary stars (LMDEB) from theoretical stellar models. Methods. We developed a physical model of the LMDEB system NSVS 10653195 to accurately measure the masses and radii of the components. We obtained several high-resolution spectra in order to fit a spectroscopic orbit. Standardized absolute photometry was obtained to measure reliable color indices and to measure the mean T of the system in out-of-eclipse phases. We observed and analyzed optical VRI and infrared JK band differential light-curves which were fitted using PHOEBE. A Markov chain Monte-Carlo (MCMC) simulation near the solution found provides robust uncertainties for the fitted parameters. Results. NSVS 10653195 is a detached eclipsing binary composed of two similar stars with masses of M = 0.6402 ± 0.0052 Mo and M = 0.6511 ± 0.0052 Mo and radii of R = 0.687 Ro and R = 0.672 Ro. Spectral types were estimated to be K6V and K7V. These stars rotate in a circular orbit with an orbital inclination of i = 86.22 ± 0.61 degrees and a period of P = 0.5607222(2) d. The distance to the system is estimated to be d = 135.2 pc, in excellent agreement with the value from Gaia. If solar metallicity were assumed, the age of the system would be older than log (age) ∼ 8 based on the M-log T diagram. Conclusions. NSVS 10653195 is composed of two oversized and active K stars. While their radii is above model predictions their T are in better agreement with models.
Bibliographic Details
http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=85069478414&origin=inward; http://dx.doi.org/10.1051/0004-6361/201935516; https://www.aanda.org/10.1051/0004-6361/201935516; https://www.aanda.org/10.1051/0004-6361/201935516/pdf; https://dx.doi.org/10.1051/0004-6361/201935516; https://www.aanda.org/articles/aa/full_html/2019/07/aa35516-19/aa35516-19.html
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