Supernovae from massive AGB stars

Abstract

We present new computations of the final fate of massive AGB-stars. These stars form ONeMg cores after a phase of carbon burning and are called Super AGB stars (SAGB). Detailed stellar evolutionary models until the thermally pulsing AGB were computed using three di erent stellar evolution codes. The subsequent evolution was modeled by a synthetic code with di erent options for mass loss rate and dredge-up e ciency. We find a range of initial masses between 9:0M and 9:25M for which we expect an SAGB star to explode as an electron capture supernova. Our models allow a detailed assessment of the envelope properties of electron-capture supernova progenitors. SAGB stars with lower initial masses are the progenitors of ONeMg white dwarf, while more massive stars ignite (o -center) neon burning and follow the classical core-collapse path.