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HD 54879 is the most recently discovered magnetic O-type star. Previousstudies ruled out a rotation period shorter than 7 years, implying that HD54879 is the second most slowly-rotating known magnetic O-type star. We reportnew high-resolution spectropolarimetric measurements of HD 54879, which confirmthat a full stellar rotation cycle has been observed, and derive a rotationperiod of $P = 2562^{+63}_{-58}$ d (about 7.02 yr). The radial velocity of HD54879 has been stable over the last decade of observations. We exploreequivalent widths and longitudinal magnetic fields calculated from lines ofdifferent elements, and conclude the atmosphere of HD 54879 is likelychemically homogeneous, with no strong evidence for chemical stratification orlateral abundance nonuniformities. We present the first detailed magnetic mapof the star, with an average surface magnetic field strength of 2954 G, and astrength for the dipole component of 3939 G. There is a significant amount ofmagnetic energy in the quadrupole components of the field (23 percent). Thus,we find HD 54879 has a strong magnetic field with a significantly complextopology.

First Observation of the Complete Rotation Period of the Ultra-Slowly Rotating Magnetic O Star HD 54879