 The radiation zone is the region of the stellar interior where the flux of energy outward is dependent on radiative heat transfer , since convective heat transfer is inefficient in that zone . In this region the plasma will not be <unk> , and any mass motions will die out . If this is not the case , however , then the plasma becomes unstable and convection will occur , forming a convection zone . This can occur , for example , in regions where very high energy <unk> occur , such as near the core or in areas with high <unk> ( making <unk> heat transfer inefficient ) as in the outer envelope . 
