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Cited by 200Gamma-ray bursts and supernovaeStellar, planetary, and galactic studiesNuclear physics research studies

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ADVANCED BURNING STAGES AND FATE OF 8-10 M☉STARS

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Jones, S., Hirschi, R., Nomoto, K., Fischer, T., Timmes, F. X., Herwig, F., Paxton, B., Toki, H., Suzuki, T., Martínez-Pinedo, G., Lam, Y. H., Bertolli, M. G.·2013·The Astrophysical Journal
DOI 10.1088/0004-637x/772/2/150
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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 Y e (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 20 Ne 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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Research works printed but not linked: 54

  1. 10.1051/0004-6361:20034328 · DOI
  2. Blöcker, 1995, A&A, 297, 727
  3. 10.1086/159670 · DOI
  4. Denissenkov, 2013, ApJ, 762, 8, 10.1088/0004-637X/762/1/8 · DOI
  5. 10.1111/j.1365-2966.2009.15772.x · DOI
  6. 10.1111/j.1745-3933.2007.00285.x · DOI
  7. 10.1111/j.1365-2966.2004.08041.x · DOI
  8. 10.1051/0004-6361/200913106 · DOI
  9. Freytag, 1996, A&A, 313, 497
  10. 10.1086/163208 · DOI
  11. Garcia-Berro, 1997, ApJ, 485, 765, 10.1086/304444 · DOI
  12. 10.1086/176934 · DOI
  13. 10.1051/0004-6361/201118643 · DOI
  14. Herwig, 2000, A&A, 360, 952
  15. 10.1146/annurev.astro.43.072103.150600 · DOI
  16. Herwig, 2007, Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes, 43
  17. Herwig, 2006, ApJ, 642, 1057, 10.1086/501119 · DOI
  18. Herwig, 2011, ApJ, 727, 89, 10.1088/0004-637X/727/2/89 · DOI · Paper page
  19. 10.1051/0004-6361:20041095 · DOI
  20. Hoffman, 2008, ApJL, 676, L127, 10.1086/587621 · DOI
  21. Iben, 1997, ApJ, 489, 772, 10.1086/304822 · DOI
  22. Janka, 2008, 40 Years of Pulsars: Millisecond Pulsars, Magnetars and More, 369
  23. Jennings, 2012, ApJ, 761, 26, 10.1088/0004-637X/761/1/26 · DOI
  24. 10.1051/0004-6361:20054703 · DOI
  25. 10.1038/nature10529 · DOI
  26. Langanke, 2000, NuPhA, 673, 481
  27. 10.1051/0004-6361/201218826 · DOI
  28. 10.1086/165368 · DOI
  29. Miyaji, 1980, PASJ, 32, 303
  30. Mocák, 2011, ApJ, 743, 55, 10.1088/0004-637X/743/1/55 · DOI
  31. Müller, 2012, ApJ, 761, 72, 10.1088/0004-637X/761/1/72 · DOI
  32. Ning, 2007, ApJL, 667, L159, 10.1086/522372 · DOI
  33. 10.1086/161749 · DOI
  34. 10.1086/165716 · DOI
  35. Nomoto, 1988, PhR, 163, 13
  36. 10.1038/299803a0 · DOI
  37. 10.1006/adnd.1994.1007 · DOI
  38. Paxton, 2011, ApJS, 192, 3, 10.1088/0067-0049/192/1/3 · DOI
  39. Poelarends, 2008, ApJ, 675, 614, 10.1086/520872 · DOI
  40. Reimers, 1975, MSRSL, 8, 369
  41. Ritossa, 1999, ApJ, 515, 381, 10.1086/307017 · DOI
  42. Schwab, 2010, ApJ, 719, 722, 10.1088/0004-637X/719/1/722 · DOI
  43. 10.1051/0004-6361:20078132 · DOI
  44. 10.1051/0004-6361/200913556 · DOI
  45. 10.1146/annurev-astro-082708-101737 · DOI
  46. Takahara, 1989, NuPhA, 504, 167
  47. 10.1086/163403 · DOI
  48. 10.1086/171746 · DOI
  49. 10.1086/173565 · DOI
  50. Toki, 2013, PhRvC
  51. Wagenhuber, 1994, A&A, 290, 807
  52. Wanajo, 2011, ApJL, 726, L15, 10.1088/2041-8205/726/2/L15 · DOI · Paper page
  53. Wanajo, 2009, ApJ, 695, 208, 10.1088/0004-637X/695/1/208 · DOI
  54. 10.1103/RevModPhys.74.1015 · DOI

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Metadata

Authors
Jones, S., Hirschi, R., Nomoto, K., Fischer, T., Timmes, F. X., Herwig, F., Paxton, B., Toki, H., Suzuki, T., Martínez-Pinedo, G., Lam, Y. H., & Bertolli, M. G.
Affiliations
  • Keele University (GB)
  • Kavli Institute for the Physics and Mathematics of the Universe (JP)
  • GSI Helmholtz Centre for Heavy Ion Research (DE)
  • University of Notre Dame (US)
  • University of California, Santa Barbara (US)
  • Research Center for Nuclear Physics, The University of Osaka (JP)
  • Nihon University (JP)
  • Technische Universität Darmstadt (DE)
  • Los Alamos National Laboratory (US)
Corresponding author
Jones, S.
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2013-07-17
Volume
772
Issue
2
Pages
150
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/772/2/150
OpenAlex
W1994768727
Cited by
200
References
0
Citations by year
2026: 8 · 2025: 10 · 2024: 12 · 2023: 9 · 2022: 10 · 2021: 12 · 2020: 16 · 2019: 17 · 2018: 25 · 2017: 35 · 2016: 14 · 2015: 14 · 2014: 15 · 2013: 3
FWCI
8.28
Type
journal article
Language
en
Open access
Licence
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
Funders
  • National Science Foundation (0922648, DE-AC52-06NA25396, 0216783, 1109174, 25915, FP/2007‐2013)
  • U.S. Department of Energy (DE-AC52-06NA2-5396, AC52-06NA25396)
  • European Commission (2007–2013, FP/2007/2013)
  • Ministry of Education, Culture, Sports, Science and Technology
  • Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung (133378, 25915, FP/2007-2013)
  • Helmholtz International Center for FAIR
  • National Nuclear Security Administration (DEAC52- 06NA25396)
  • Science and Technology Facilities Council (ST/J000035/1, PP/F000057/1, PP/D000955/1, ST/G002355/1)
  • Japan Society for the Promotion of Science (22540290, 23224004)
  • Los Alamos National Laboratory (AC52-06NA25396, DE-AC52-06NA25396)
  • FP7 Ideas: European Research Council (306901)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Nuclear physics research studies
Keywords
super-AGB stars, electron-capture supernovae, supernova progenitors, Urca processes, thermal pulses, massive star evolution, neutron star mass distribution

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CoChat. (2026). Citation check: ADVANCED BURNING STAGES AND FATE OF 8-10 M☉STARS. https://app.cochat.ai/papers/10.1088/0004-637x/772/2/150
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Jones, S., Hirschi, R., Nomoto, K., Fischer, T., Timmes, F. X., Herwig, F., Paxton, B., Toki, H., Suzuki, T., Martínez-Pinedo, G., Lam, Y. H., & Bertolli, M. G. (2013). ADVANCED BURNING STAGES AND FATE OF 8-10 M☉STARS. The Astrophysical Journal. https://doi.org/10.1088/0004-637x/772/2/150