Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition
Recent literature on core-collapse supernovae suggests that a black hole (BH) can form within ∼1 s of shock revival, while still culminating in a successful supernova. We refer to these as BH supernovae, as they are distinct from other BH formation channels in both timescale and impact on the explos...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada899 |
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| author | Oliver Eggenberger Andersen Evan O’Connor Haakon Andresen André da Silva Schneider Sean M. Couch |
| author_facet | Oliver Eggenberger Andersen Evan O’Connor Haakon Andresen André da Silva Schneider Sean M. Couch |
| author_sort | Oliver Eggenberger Andersen |
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| description | Recent literature on core-collapse supernovae suggests that a black hole (BH) can form within ∼1 s of shock revival, while still culminating in a successful supernova. We refer to these as BH supernovae, as they are distinct from other BH formation channels in both timescale and impact on the explosion. We simulate these events self-consistently from core collapse until 20–50 days after collapse using three axisymmetric models of a 60 M _⊙ zero-age main-sequence progenitor star and investigate how the composition of the ejecta is impacted by the BH formation. We employ Skyrme-type equations of state (EOSs) and vary the uncertain nucleonic effective mass, which affects the pressure inside the proto–neutron star through the thermal part of the EOS. This results in different BH formation times and explosion energies at BH formation, yielding final explosion energies between 0.06 and 0.72 × 10 ^51 erg with 21.8–23.3 M _⊙ of ejecta, of which 0–0.018 M _⊙ is ^56 Ni. Compared to expectations from 1D simulations, we find more nuanced EOS dependences of the explosion dynamics, the mass of the BH remnant, and the elemental composition of the ejecta. We investigate why the explosions survive despite the massive overburden and link the shape of the diagnostic energy curve and character of the ejecta evolution to the progenitor structure. |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-9d37457e1af344efbc3209bd539763782025-02-04T07:40:34ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198015310.3847/1538-4357/ada899Black Hole Supernovae, Their Equation of State Dependence, and Ejecta CompositionOliver Eggenberger Andersen0https://orcid.org/0000-0002-9660-7952Evan O’Connor1https://orcid.org/0000-0002-8228-796XHaakon Andresen2https://orcid.org/0000-0002-4747-8453André da Silva Schneider3https://orcid.org/0000-0003-0849-7691Sean M. Couch4https://orcid.org/0000-0002-5080-5996The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-106 91 Stockholm, Sweden ; oliver.e.andersen@astro.su.seThe Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-106 91 Stockholm, Sweden ; oliver.e.andersen@astro.su.seThe Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-106 91 Stockholm, Sweden ; oliver.e.andersen@astro.su.seDepartamento de Física, Universidade Federal de Santa Catarina , Florianópolis, SC 88040-900, BrazilDepartment of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA; Department of Computational Mathematics, Science, and Engineering, Michigan State University , East Lansing, MI 48824, USA; Facility for Rare Isotope Beams, Michigan State University , East Lansing, MI 48824, USARecent literature on core-collapse supernovae suggests that a black hole (BH) can form within ∼1 s of shock revival, while still culminating in a successful supernova. We refer to these as BH supernovae, as they are distinct from other BH formation channels in both timescale and impact on the explosion. We simulate these events self-consistently from core collapse until 20–50 days after collapse using three axisymmetric models of a 60 M _⊙ zero-age main-sequence progenitor star and investigate how the composition of the ejecta is impacted by the BH formation. We employ Skyrme-type equations of state (EOSs) and vary the uncertain nucleonic effective mass, which affects the pressure inside the proto–neutron star through the thermal part of the EOS. This results in different BH formation times and explosion energies at BH formation, yielding final explosion energies between 0.06 and 0.72 × 10 ^51 erg with 21.8–23.3 M _⊙ of ejecta, of which 0–0.018 M _⊙ is ^56 Ni. Compared to expectations from 1D simulations, we find more nuanced EOS dependences of the explosion dynamics, the mass of the BH remnant, and the elemental composition of the ejecta. We investigate why the explosions survive despite the massive overburden and link the shape of the diagnostic energy curve and character of the ejecta evolution to the progenitor structure.https://doi.org/10.3847/1538-4357/ada899Core-collapse supernovaeSupernovaeBlack holesHydrodynamical simulationsRadiative transfer simulationsNeutron stars |
| spellingShingle | Oliver Eggenberger Andersen Evan O’Connor Haakon Andresen André da Silva Schneider Sean M. Couch Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition The Astrophysical Journal Core-collapse supernovae Supernovae Black holes Hydrodynamical simulations Radiative transfer simulations Neutron stars |
| title | Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition |
| title_full | Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition |
| title_fullStr | Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition |
| title_full_unstemmed | Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition |
| title_short | Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition |
| title_sort | black hole supernovae their equation of state dependence and ejecta composition |
| topic | Core-collapse supernovae Supernovae Black holes Hydrodynamical simulations Radiative transfer simulations Neutron stars |
| url | https://doi.org/10.3847/1538-4357/ada899 |
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