Simulations Show Disk-Bounce Ejecta from Rotating Supermassive Star Collapse
Rotating very massive star collapses can launch massive, energetic outflows whose composition depends on core mass. The work uses full numerical relativity plus nuclear burning, yet remains purely theoretical and omits magnetic fields and realistic progenitor rotation profiles. Future multimessenger searches for unusually luminous, iron-rich transients could test the predicted ejecta.
The study ran general-relativistic hydrodynamics plus neutrino cooling and a 13-isotope alpha network on newly constructed rotating cores. Lower-mass pair-unstable models reached higher central densities before collapse, allowing efficient neutrino losses that left more mass outside the initial black hole and enabled a massive, high-angular-momentum disk. Higher-mass GR-unstable cores collapsed more homologously, forming smaller disks and less energetic ejecta. Viscosity-driven follow-up runs showed further mass ejection once the disk reached nuclear statistical equilibrium.
Fujibayashi: No 56Ni-rich kilonova-like transient from >10^4 solar-mass collapses detected by LSST within three years of operations.
Sources (2)
- [1]Primary Source(https://arxiv.org/abs/2608.13642)
- [2]Supporting Source(https://arxiv.org/abs/2305.13377)