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The hot WN star WR2 (HD6327) has been claimed to have many singularcharacteristics. To explain its unusually rounded and relatively weak emissionline profiles, it has been proposed that WR2 is rotating close to break-up witha magnetically confined wind. Alternatively, the line profiles could beexplained by the dilution of WR2's spectrum by that of a companion. In thispaper, we present a study of WR2 using near-infrared AO imaging and opticalspectroscopy and polarimetry. Our spectra reveal the presence of weakphotospheric absorption lines from a ~B2.5-4V companion, which howevercontributes only ~5-10% to the total light, suggesting that the companion is abackground object. Therefore, its flux cannot be causing any significantdilution of the WR star's emission lines. The absence of intrinsic linearcontinuum polarization from WR2 does not support the proposed fast rotation.Our Stokes V spectrum was not of sufficient quality to test the presence of amoderately strong organized magnetic field but our new modelling indicates thatto confine the wind the putative magnetic field must be significantly strongerthan was previously suggested sufficiently strong as to make its presenceimplausible.

Investigating the origin of the spectral line profiles of the Hot Wolf-Rayet Star WR2