Context : Results from the theory of radiatively driven winds are nowadays incorporated in stellar evolutionary and population synthesis models , and are used in our interpretation of the observations of the deep Universe .
Yet , the theory has been confirmed only until Small Magellanic Cloud ( SMC ) metallicities .
Observations and analyses of O-stars at lower metallicities are difficult , but much needed to prove the theory .

Aims : We have observed GHV-62024 , an O6.5 IIIf star in the low-metallicity galaxy IC 1613 ( Z \approx 0.15 Z _ { \odot } ) to study its evolution and wind .
According to a previous preliminary analysis that was subject to significant restrictions this star could challenge the radiatively driven wind theory at low metallicities .
Here we present a complete analysis of this star .

Methods : Our observations were obtained with VIMOS at VLT , at R \approx 2000 and covered approximately between 4000 and 7000 Å .
The observations were analysed using the latest version of the model atmosphere code FASTWIND , which includes the possibility of calculating the N iii spectrum

Results : We obtain the stellar parameters and conclude that the star follows the average wind momentum–luminosity relationship ( WLR ) expected for its metallicity , but with a high value for the exponent of the wind velocity law , \beta .
Comparing this with values of other stars in the literature , we suggest that this high value may be reached because GHV-62024 could be a fast rotator seen at a low inclination angle .
We also suggest that this could favour the appearance of the spectral ” f ” -characterictics .
While the derived \beta value does not change by adopting a lower wind terminal velocity , we show that a wrong V _ { \infty } has a clear impact on the position of the star in the WLR diagram .
The N and He abundances are very high , consistent with strong CNO mixing that could have been caused by the fast rotation , although we can not discard a different origin with present data .
Stellar evolutionary model predictions are consistent with the star being still a fast rotator .
We find again the well-known mass-discrepancy for this star .

Conclusions : We conclude that the star follows the WLR expected for its metallicity .
The results are consistent with GHV-62024 being a fast rotator seen close to pole-on , strongly contaminated at the surface with CNO products and with a wind structure altered by the fast rotation but without modifying the global WLR .
We suggest that this could be a general property of fast rotators .