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We present observations and analysis of an RS CVn-type double-lined eclipsingbinary system, RU Cnc. The system has been observed for over a century. Thehigh-quality long-cadence \emph{Kepler} K2 C5 and C18, newly obtainedobservations, and two radial velocity curves were combined and analyzedsimultaneously assuming multi-spot model. The masses, radii and luminosities ofthe component stars are precisely obtained as $M_\textrm{c} = 1.386\pm0.044\,M_{_\odot}$, $M_\textrm{h} = 1.437 \pm 0.046\, M{_\odot}$, $R_\textrm{h} =2.39\pm 0.07\, R{_\odot}$, $R_\textrm{c} = 5.02 \pm 0.08\, R{_\odot}$,$L_\textrm{h} = 11.4\pm 1.2\, L{_\odot}$, $L_\textrm{c} = 12.0 \pm 1.0\,L{_\odot}$ and with a separation of $\textrm{a} = 27.914 \pm 0.016\,R{_\odot}$. The distance of the system is determined to be $380\pm 57\,$ pcwhich is consistent with the Gaia DR2 result. Long-term detailed periodvariation analysis of the system indicate a period decrease of$7.9\times10^{-7}$ days per year. The results suggest the cooler component tobe on the red giant branch (RGB) and the hotter one to be still on the mainsequence.

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