Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition

Journal Article · 03 February 2025 · The Astrophysical Journal

DOI: https://doi.org/10.3847/1538-4357/ada899 · OSTI ID:2510892

Eggenberger Andersen, Oliver ; O’Connor, Evan ; Andresen, Haakon ; da Silva Schneider, André ; Couch, Sean M.

Abstract 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.

• Sponsoring Organization: USDOE
• Grant/Contract Number: SC0017955
• OSTI ID: 2510892
• Journal Information: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 1 Vol. 980; ISSN 0004-637X
• Publisher: American Astronomical SocietyCopyright Statement
• Country of Publication: United States
• Language: English