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Aims: Following our comprehensive studies of the WR stars in the Milky Way,we now present spectroscopic analyses of almost all known WN stars in the LMC.Methods: For the quantitative analysis of the wind-dominated emission-linespectra, we employ the Potsdam Wolf-Rayet (PoWR) model atmosphere code. Byfitting synthetic spectra to the observed spectral energy distribution and theavailable spectra (ultraviolet and optical), we obtain the physical propertiesof 107 stars. Results: We present the fundamental stellar and wind parametersfor an almost complete sample of WN stars in the LMC. Among those stars thatare putatively single, two different groups can be clearly distinguished. While12% of our sample are more luminous than 10^6 Lsun and contain a significantamount of hydrogen, 88% of the WN stars, with little or no hydrogen, populatethe luminosity range between log (L/Lsun) = 5.3...5.8. Conclusions: While thefew extremely luminous stars (log (L/Lsun) > 6), if indeed single stars,descended directly from the main sequence at very high initial masses, the bulkof WN stars have gone through the red-supergiant phase. According to theirluminosities in the range of log (L/Lsun) = 5.3...5.8, these stars originatefrom initial masses between 20 and 40 Msun. This mass range is similar to theone found in the Galaxy, i.e. the expected metallicity dependence of theevolution is not seen. Current stellar evolution tracks, even when accountingfor rotationally induced mixing, still partly fail to reproduce the observedranges of luminosities and initial masses. Moreover, stellar radii aregenerally larger and effective temperatures correspondingly lower thanpredicted from stellar evolution models, probably due to subphotosphericinflation.

The Wolf-Rayet stars in the Large Magellanic Cloud: A comprehensive analysis of the WN class