Advanced burning stages and fate of 8-10 M STARS

S. Jones, R. Hirschi, K. Nomoto, T. Fischer, Francis Timmes, F. Herwig, B. Paxton, H. Toki, T. Suzuki, G. Martínez-Pinedo, Y. H. Lam, M. G. Bertolli

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Abstract

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.

Original languageEnglish (US)
Article number150
JournalAstrophysical Journal
Volume772
Issue number2
DOIs
StatePublished - Aug 1 2013

Fingerprint

neon
supernovae
electron capture
asymptotic giant branch stars
electron
shell
M stars
massive stars
iron
M region
chemical evolution
galactic evolution
pulses
stellar mass
mass distribution
neutron stars
oxygen

Keywords

  • nuclear reactions, nucleosynthesis, abundances
  • stars: AGB and post-AGB
  • stars: evolution
  • stars: neutron
  • supernovae: general

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Jones, S., Hirschi, R., Nomoto, K., Fischer, T., Timmes, F., Herwig, F., ... Bertolli, M. G. (2013). Advanced burning stages and fate of 8-10 M STARS. Astrophysical Journal, 772(2), [150]. https://doi.org/10.1088/0004-637X/772/2/150

Advanced burning stages and fate of 8-10 M STARS. / Jones, S.; Hirschi, R.; Nomoto, K.; Fischer, T.; Timmes, Francis; Herwig, F.; Paxton, B.; Toki, H.; Suzuki, T.; Martínez-Pinedo, G.; Lam, Y. H.; Bertolli, M. G.

In: Astrophysical Journal, Vol. 772, No. 2, 150, 01.08.2013.

Research output: Contribution to journalArticle

Jones, S, Hirschi, R, Nomoto, K, Fischer, T, Timmes, F, Herwig, F, Paxton, B, Toki, H, Suzuki, T, Martínez-Pinedo, G, Lam, YH & Bertolli, MG 2013, 'Advanced burning stages and fate of 8-10 M STARS', Astrophysical Journal, vol. 772, no. 2, 150. https://doi.org/10.1088/0004-637X/772/2/150
Jones S, Hirschi R, Nomoto K, Fischer T, Timmes F, Herwig F et al. Advanced burning stages and fate of 8-10 M STARS. Astrophysical Journal. 2013 Aug 1;772(2). 150. https://doi.org/10.1088/0004-637X/772/2/150
Jones, S. ; Hirschi, R. ; Nomoto, K. ; Fischer, T. ; Timmes, Francis ; Herwig, F. ; Paxton, B. ; Toki, H. ; Suzuki, T. ; Martínez-Pinedo, G. ; Lam, Y. H. ; Bertolli, M. G. / Advanced burning stages and fate of 8-10 M STARS. In: Astrophysical Journal. 2013 ; Vol. 772, No. 2.
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abstract = "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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