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Title: ADVANCED BURNING STAGES AND FATE OF 8-10 M{sub Sun} STARS

The stellar mass range 8 {approx}< M/M{sub Sun} {approx}< 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{sub Sun} 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{sub Sun} model, however, fails to reach the center as the URCA process and an extended (0.6 M{sub Sun }) region of low Y{sub 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 pulsesmore » (TPs). We also present models of an 8.75 M{sub Sun} SAGB star through its entire TP phase until electron captures on {sup 20}Ne begin at its center and of a 12 M{sub Sun} 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.« less
Authors:
;  [1] ;  [2] ; ;  [3] ;  [4] ;  [5] ;  [6] ;  [7] ;  [8] ;  [9] ;  [10]
  1. Astrophysics Group, Lennard Jones Building, Keele University, Staffordshire ST5 5BG (United Kingdom)
  2. Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa, Chiba 277-8583 (Japan)
  3. GSI Helmholtzzentrum fuer Schwerionenforschung GmbH, Planckstrasse 1, D-64291 Darmstadt (Germany)
  4. School of Earth and Space Exploration, University of Arizona, Tempe, AZ 85287 (United States)
  5. Joint Institute for Nuclear Astrophysics, University of Notre Dame, IN 46556 (United States)
  6. KITP and Department of Physics, University of California, Santa Barbara, CA 93106 (United States)
  7. Research Center for Nuclear Physics (RCNP), Osaka University, Osaka 567-0047 (Japan)
  8. Department of Physics, College of Humanities and Sciences, Nihon University Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550 (Japan)
  9. Institut fuer Kernphysik, Technische Universitaet Darmstadt, Schlossgartenstrasse 2, D-64289 Darmstadt (Germany)
  10. Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)
Publication Date:
OSTI Identifier:
22121773
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 772; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ELECTRON CAPTURE; IRON; MASS DISTRIBUTION; NEON; NEON 20; NEUTRON STARS; OXYGEN; STAR BURNING; SUPERNOVAE