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We present the results of the combined photometric and spectroscopic analysisof a bright (V=9.14), nearby (d=31 pc), late-type detached eclipsing binary AKFornacis. This P=3.981 d system has not been previously recognised as adouble-lined spectroscopic binary, and this is the first full physical model ofthis unique target. With the FEROS, CORALIE and HARPS spectrographs wecollected a number of high-resolution spectra in order to calculate radialvelocities of both components of the binary. Measurements were done with ourown disentangling procedure and the TODCOR technique, and were later combinedwith the photometry from the ASAS and SuperWASP archives. We also performed anatmospheric analysis of the component spectra with the Spectroscopy Made Easy(SME) package. Our analysis shows that AK For consists of two active, cooldwarfs having masses of $M_1=0.6958 \pm 0.0010$ and $M_2=0.6355 \pm 0.0007$M$_\odot$ and radii of $R_1=0.687 \pm 0.020$ and $R_2=0.609 \pm 0.016$R$_\odot$, slightly less metal abundant than the Sun. Parameters of bothcomponents are well reproduced by the models.  AK For is the brightest system among the known eclipsing binaries with K or Mtype stars. Its orbital period is one of the longest and rotational velocitiesone of the lowest, which allows us to obtain very precise radial velocitymeasurements. The precision in physical parameters we obtained places AK Foramong the binaries with the best mass measurements in the literature. It alsofills the gap in our knowledge of stars in the range of 0.5-0.8 M$_\odot$, andbetween short and long-period systems. All this makes AK For a unique benchmarkfor understanding the properties of low-mass stars.

astronomy and astrophysics

Orbital and physical parameters of eclipsing binaries from the All-Sky  Automated Survey catalogue - VI. AK Fornacis - a rare, bright K-type  eclipsing binary