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During their main sequence evolution, massive stars can develop convectiveregions very close to their surface. These regions are caused by an opacitypeak associated with iron ionization. Cantiello et al. (2009) found a possibleconnection between the presence of sub-photospheric convective motions andsmall scale stochastic velocities in the photosphere of early-type stars. Thissupports a physical mechanism where microturbulence is caused by waves that aretriggered by subsurface convection zones. They further suggest that clumping inthe inner parts of the winds of OB stars could be related to subsurfaceconvection, and that the convective layers may also be responsible forstochastic excitation of non-radial pulsations. Furthermore, magnetic fieldsproduced in the iron convection zone could appear at the surface of suchmassive stars. Therefore subsurface convection could be responsible for theoccurrence of observable phenomena such as line profile variability anddiscrete absorption components. These phenomena have been observed for decades,but still evade a clear theoretical explanation. Here we present preliminaryresults from 3D MHD simulations of such subsurface convection.

3D MHD simulations of subsurface convection in OB stars