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The Wolf-Rayet star Mk 34 was observed more than 50 times as part of the deepT-ReX Chandra ACIS-I X-ray imaging survey of the Tarantula Nebula in the LargeMagellanic Cloud conducted between 2014 May and 2016 January. Its brightnessshowed one bright maximum and repeated faint minima which help define an X-rayrecurrence time of $155.1\pm0.1$ days that is probably the orbital period of aneccentric binary system. The maximum immediately precedes the minimum in thefolded X-ray light curve as confirmed by new Swift XRT observations.Notwithstanding its extreme median luminosity of$1.2\times10^{35}\mathrm{erg}~\mathrm{s}^{-1}$, which makes it over an order ofmagnitude brighter than comparable stars in the Milky Way, Mk 34 is almostcertainly a colliding-wind binary system. Its spectrum shows phase-relatedchanges of luminosity and absorption that are probably related to the orbitaldynamics of two of the most massive stars known.

The 155-day X-ray cycle of the very massive Wolf-Rayet star Melnick 34 in the Large Magellanic Cloud