Higher-Mach-number self-similar shock solutions in failed supernovae are unstable and strengthen asymptotically above a critical neutrino mass-loss threshold, explaining greater ejection in red supergiants versus compact progenitors.
Delayed explosions of red supergiants following 'failed' supernovae
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Black hole progenitors are predominantly hot and blue at pre-collapse, often Wolf-Rayet stars luminous in ultraviolet, with only a minority as red supergiants, and a direct-collapse rate of about 0.4 per century for a galaxy with 1 solar mass per year star formation.
Hydrodynamic simulations of three jet pairs in the jittering-jets mechanism reproduce the ring-and-bar morphology of supernova remnant G11.2-0.3.
N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.
citing papers explorer
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On the Origin of Mass Ejection in Failed Supernovae
Higher-Mach-number self-similar shock solutions in failed supernovae are unstable and strengthen asymptotically above a critical neutrino mass-loss threshold, explaining greater ejection in red supergiants versus compact progenitors.
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Hot blue progenitors of stellar-mass black holes
Black hole progenitors are predominantly hot and blue at pre-collapse, often Wolf-Rayet stars luminous in ultraviolet, with only a minority as red supergiants, and a direct-collapse rate of about 0.4 per century for a galaxy with 1 solar mass per year star formation.
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Simulating the jittering-jets explosion mechanism: Supernova remnant G11.2-0.3
Hydrodynamic simulations of three jet pairs in the jittering-jets mechanism reproduce the ring-and-bar morphology of supernova remnant G11.2-0.3.
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The neighboring stars of N6946-BH1 and the observational characteristics of failed supernovae
N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.