From the composition of early Solar System condensates it is well know that now-extinct short-lived radionuclides (SLR) were present at the time when these condensates formed . One of the current scenario for the origin of these SLRs involves an external stellar source to have polluted the early Solar System. One main issue with this scenario is to find an appropriate source that could generate the unique pattern as seen in the SLRs [see, e.g., 2]. We investigate the production of SLRs in a nearby Super Asymptotic Giant Branch (SAGB) star, including for the first time the radionuclides heavier than Fe. SAGB stars have initial stellar masses in the range of ~ 7–11 solar masses [3,4]. They burn H, He, and C in their core, but do not experience further core burning. After core C burning they go through the SAGB phase, with the H and He shells activated alternately, episodic thermal pulses in the He shell, and strong stellar winds driving the H-rich envelope into the surrounding interstellar medium. The final remnants of the evolution of SAGB stars are mostly O-Ne white dwarfs, although electron capture supernovae could also occur.
|Number of pages||1|
|Publication status||Published - 2012|
|Event||Annual Meeting of the Meteoritical-Society 2012 - Cairns, Australia|
Duration: 12 Aug 2012 → 17 Aug 2012
Conference number: 75th
|Conference||Annual Meeting of the Meteoritical-Society 2012|
|Period||12/08/12 → 17/08/12|
Doherty, C. L., Lugaro, M., Lau, H., Siess, L., Lattanzio, J. C., & Gil-Pons, P. (2012). Production of short-lived radioactive nuclei in super asymptotic giant branch stars. Poster session presented at Annual Meeting of the Meteoritical-Society 2012, Cairns, Australia.