We provide mass-loss rate predictions for O stars from Large and Small Magellanic Clouds .
We calculate global ( unified , hydrodynamic ) model atmospheres of main sequence , giant , and supergiant stars for chemical composition corresponding to Magellanic Clouds .
The models solve radiative transfer equation in comoving frame , kinetic equilibrium equations ( also known as NLTE equations ) , and hydrodynamical equations from ( quasi- ) hydrostatic atmosphere to expanding stellar wind .
The models allow us to predict wind density , velocity , and temperature ( consequently also the terminal wind velocity and the mass-loss rate ) just from basic global stellar parameters .
As a result of their lower metallicity , the line radiative driving is weaker leading to lower wind mass-loss rates with respect to the Galactic stars .
We provide a formula that fits the mass-loss rate predicted by our models as a function of stellar luminosity and metallicity .
On average , the mass-loss rate scales with metallicity as \dot { M } \sim Z ^ { 0.59 } .
The predicted mass-loss rates are lower than mass-loss rates derived from H \alpha diagnostics and can be reconciled with observational results assuming clumping factor C _ { \text { c } } = 9 .
On the other hand , the predicted mass-loss rates either agree or are slightly higher than the mass-loss rates derived from ultraviolet wind line profiles .
The calculated P v ionization fractions also agree with values derived from observations for LMC stars with T _ { \text { eff } } \leq 40 000 K. Taken together , our theoretical predictions provide reasonable models with consistent mass-loss rate determination , which can be used for quantitative study of stars from Magellanic Clouds .