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We present a first and detailed study of the bright and active K0IV-III starHD 123351. The star is found to be a single-lined spectroscopic binary with aperiod of 147.8919+-0.0003 days and a large eccentricity of e=0.8086+-0.0001.The rms of the orbital solution is just 47 m/s, making it the most preciseorbit ever obtained for an active binary system. The rotation period isconstrained from long-term photometry to be 58.32+-0.01 days. It shows that HD123351 is a very asynchronous rotator, rotating five times slower than theexpected pseudo-synchronous value. Two spotted regions persisted throughout the12 years of our observations. Four years of Halpha, CaII H&K and HeI D3monitoring identifies the same main periodicity as the photometry but dynamicspectra also indicate that there is an intermittent dependence on the orbitalperiod, in particular for Ca ii H&K in 2008. Line-profile inversions of a pairof Zeeman sensitive/insensitive iron lines yield an average surfacemagnetic-flux density of 542+-72 G. The time series for 2008 is modulated bythe stellar rotation as well as the orbital motion, such that the magnetic fluxis generally weaker during times of periastron and that the chromosphericemissions vary in anti-phase with the magnetic flux. We also identify a broadand asymmetric lithium line profile and measure an abundance of log n(Li) =1.70+-0.05. The star's position in the H-R diagram indicates a mass of 1.2+-0.1Msun and an age of 6-7 Gyr. We interpret the anti-phase relation of themagnetic flux with the chromospheric emissions as evidence that there are twomagnetic fields present at the same time, a localized surface magnetic fieldassociated with spots and a global field that is oriented towards the(low-mass) secondary component.

Binary-induced magnetic activity? Time-series echelle spectroscopy and photometry of HD123351 = CZ CVn