  The magnetic fields, activity and dynamos of young solar-type stars can be
empirically studied using time-series of spectropolarimetric observations and
tomographic imaging techniques such as Doppler imaging and Zeeman Doppler
imaging. In this paper we use these techniques to study the young Sun-like star
EK Draconis (Sp-Type: G1.5V, HD 129333) using ESPaDOnS at the
Canada-France-Hawaii Telescope and NARVAL at the T\`elescope Bernard Lyot. This
multi-epoch study runs from late 2006 until early 2012. We measure high levels
of chromospheric activity indicating an active, and varying, chromosphere.
Surface brightness features were constructed for all available epochs. The
2006/7 and 2008 data show large spot features appearing at
intermediate-latitudes. However, the 2012 data indicate a distinctive polar
spot. We observe a strong, almost unipolar, azimuthal field during all epochs
that is similar to that observed on other Sun-like stars. Using magnetic
features, we determined an average equatorial rotational velocity, \Omega_eq,
of 2.50 +/- 0.08 rad/d. High levels of surface differential rotation were
measured with an average rotational shear, \Delta\Omega, of 0.27 +0.24-0.26
rad/d. During an intensively observed 3-month period from December 2006 until
February 2007, the magnetic field went from predominantly toroidal ( approx.
80%) to a more balanced poloidal-toroidal (approx. 40-60%) field. Although the
large-scale magnetic field evolved over the epochs of our observations, no
polarity reversals were found in our data.
