star’s life, such as the core-collapse supernova paradigm, which begins with the collapse of the iron core of an evolved massive star in the end of its thermonuclear evolution (for a comprehensive review, see e.g. [@bet90]). Whether a model yields a successful explosion still challenges theorists and their numerical simulations. It is currently believed that the prompt shock, which results from the inner core’s rebound after an implosion has compressed the inner core to supranuclear density, can not propagate directly outward and expel the entire envelope, but may stall and turn into an accretion shock at a radius of 100-200 km from the explosion center due to nuclear dissociation and neutrino cooling. It is a consensus now among different groups of supernova studies, that a successful explosion model requires a so-called “shock reheating mechanism” or “delayed mechanism”[@wil85bw85], in which the neutrinos produced from the core are absorbed and/or scattered by the materials in the stalled shock and the shock could be revived to expel the envelope and give rise to a successful explosion. Many current researches on core-collapse supernova mechanisms are focused on the role of convection in the unstable regions below or above the neutrinosphere, and it seems that 