Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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Simulations predict time-dependent gamma-ray lines from r-process and iron-peak decays in accretion-induced white dwarf collapse, detectable to ~10 Mpc and absent in neutron star mergers.
Accretion-induced failure of the neutron star crystal crust produces a glass layer that explains the observed cooling, fixes the accreted mass at 2.4e-6 solar masses, and indicates birth properties typical of recycled neutron stars, potentially from electron-capture supernova formation.
A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.
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Observational signatures of thermonuclear electron-capture supernovae -- Ne II line strengthening and color evolution as traces of the explosion mechanism
Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.