Absolute properties of RU Cnc revisited: An active RS CVn-type eclipsing binary with a red giant branch and a main sequence components

Abstract

We present observations and analysis of an RS CVn-type double-lined eclipsing binary system, RU Cnc. The system has been observed for over a century. The high-quality long-cadence \emph{Kepler} K2 C5 and C18, newly obtained observations, and two radial velocity curves were combined and analyzed simultaneously assuming multi-spot model. The masses, radii and luminosities of the component stars are precisely obtained as $M_{\text{c}}=1.386\pm 0.044M_{{}_{\odot }}$, $M_{\text{h}}=1.437\pm 0.046M{}_{\odot }$, $R_{\text{h}}=2.39\pm 0.07R{}_{\odot }$, $R_{\text{c}}=5.02\pm 0.08R{}_{\odot }$, $L_{\text{h}}=11.4\pm 1.2L{}_{\odot }$, $L_{\text{c}}=12.0\pm 1.0L{}_{\odot }$ and with a separation of $\text{a}=27.914\pm 0.016R{}_{\odot }$. The distance of the system is determined to be $380\pm 57$ pc which is consistent with the Gaia DR2 result. Long-term detailed period variation analysis of the system indicate a period decrease of $7.9\times 10^{-7}$ days per year. The results suggest the cooler component to be on the red giant branch (RGB) and the hotter one to be still on the main sequence.

arXiv comment7 pages, 5 figures, 6 tables. Accepted for publication in MNRAS

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