Neutrino-driven supernovae: An accretion instability in a nuclear physics controlled environment
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Theory of core-collapse supernovae
2007, Physics ReportsCitation Excerpt :The shock is weakened so much that it finally stalls and turns into an accretion shock at a radius between 100 and 200 km, i.e., the matter downstream of the shock has negative velocities and continues falling inward (Fig. 1, middle right panel). All state-of-the-art simulations of stellar core collapse performed in Newtonian gravity [8,9], with an approximative treatment of general relativity [10–12], in full general relativity [13–17], and with stiff or soft nuclear equations of state currently available for core-collapse simulations [18–21] (see also Section 2.1) agree with the models of the 1980's and 1990's (e.g., [22–25]) that the prompt shock is unable to trigger supernova explosions.1 After the core bounce, a compact remnant begins to form at the center of the collapsing star, rapidly growing by the accretion of infalling stellar material until the explosion sets in.
Nuclear physics with spherically symmetric supernova models
2008, Journal of Physics G: Nuclear and Particle PhysicsMulti-dimensional simulations of core-collapse supernova explosions with CHIMERA
2018, AIP Conference ProceedingsEssential ingredients in core-collapse supernovae
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This work was supported by the Sonderforschungsbereich (SFB) 375 “Astro-Particle Physics” and by the SFB-Transregio 7 “Gravitational Wave Astronomy” of the Deutsche Forschungsgemeinschaft.