Discussion

We revisit the efforts of previous work on GR instability supernovae and contrast our approach and results with such studies. We highlight the importance of the GR stability analysis in determining the fate of the supermassive star, as stellar evolution codes cannot reliably find the GR radial instability. We then discuss shortcomings and sources of error associated with our approach, in HOSHI, the GR stability analysis, the hydrodynamics calculations, and the radiation hydrodynamics, respectively.