Theoretical instability domains in the upper part of the HR diagram

Massive stars are characterized by a large radiation over gaz pressure ratio and a large temperature over density ratio. With increasing stellar initial mass, they suffer stronger stellar winds which plays an important role in the chemical enrichment of the galaxies. The induced mass loss affects also the evolution and internal structure of massive stars on the main sequence (MS) and on the post-main sequence phase (post-MS). Recent ground-based observations and space missions have shown the presence of pulsations in massive stars, such as accouctic and gravity modes excited by the $\kappa$-mechanism and even solar-like oscillations. Strange modes could also found to be excited in the most massive stars. $\kappa$-mechanism instability domains are presented for the upper HR diagram (up to $70$M$_{odot}$) on the MS and on the post-MS. We compute evolutionary tracks and non-adiabatic frequencies for different input parameters such as the metallicity, the mass loss rate and the overshooting parameter.