2013ApJ...772..150J -
Astrophys. J., 772, 150 (2013/August-1)
Advanced burning stages and fate of 8-10 M☉Stars.
JONES S., HIRSCHI R., NOMOTO K., FISCHER T., TIMMES F.X., HERWIG F., PAXTON B., TOKI H., SUZUKI T., MARTINEZ-PINEDO G., LAM Y.H. and BERTOLLI M.G.
Abstract (from CDS):
The stellar mass range 8 ≲ M/M☉ ≲ 12 corresponds to the most massive asymptotic giant branch (AGB) stars and the most numerous massive stars. It is host to a variety of supernova (SN) progenitors and is therefore very important for galactic chemical evolution and stellar population studies. In this paper, we study the transition from super-AGB (SAGB) star to massive star and find that a propagating neon-oxygen-burning shell is common to both the most massive electron capture supernova (EC-SN) progenitors and the lowest mass iron-core-collapse supernova (FeCCSN) progenitors. Of the models that ignite neon-burning off-center, the 9.5 M☉star would evolve to an FeCCSN after the neon-burning shell propagates to the center, as in previous studies. The neon-burning shell in the 8.8 M☉ model, however, fails to reach the center as the URCA process and an extended (0.6 M☉) region of low Ye(0.48) in the outer part of the core begin to dominate the late evolution; the model evolves to an EC-SN. This is the first study to follow the most massive EC-SN progenitors to collapse, representing an evolutionary path to EC-SN in addition to that from SAGB stars undergoing thermal pulses (TPs). We also present models of an 8.75 M☉ SAGB star through its entire TP phase until electron captures on 20Ne begin at its center and of a 12 M☉ star up to the iron core collapse. We discuss key uncertainties and how the different pathways to collapse affect the pre-SN structure. Finally, we compare our results to the observed neutron star mass distribution.
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Journal keyword(s):
nuclear reactions, nucleosynthesis, abundances - stars: AGB and post-AGB - stars: evolution - stars: neutron - supernovae: general
Simbad objects:
2
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