  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 non-negligibly contributes to energy transfer. Indeed, instability
of modes excited at the Fe bump is likely to be suppressed with TDC compared
with the case of adopting the frozen-in convection approximation. But we make
sure that unstable strange-modes certainly appear 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.
