We carry out a nonadiabatic analysis of strange-modes in hot massive stars with time-dependent convection ( TDC ) .
In envelopes of such stars , convective luminosity is not so dominant as that in envelopes of stars in the redder side of the classical instability strip .
Around the Fe opacity bump , however , convection contributes non-negligibly to energy transfer .
Indeed , we find that instability of modes excited at the Fe bump is likely to be weaker with TDC compared with the case of adopting the frozen-in convection approximation .
But we confirm that unstable strange-modes certainly remain in hot massive stars even by taking into account TDC .
We also examine properties of the strange-mode instability , which is related to destabilization of strange-modes without adiabatic counterparts .
In this type of instability , the phase lag between density and pressure varies from 0 to 180 ^ { \circ } in an excitation zone unlike the case of the \kappa -mechanism .
In addition , we confirm by comparing models with Z = 0 and Z = 0.02 that dominance of radiation pressure is important for this type of instability .