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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AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
MOFAT applied to SN2024ggi shows CO triggering inner SiO formation with a receding edge, order-of-magnitude mass drop, clumping signatures, and no dust formation.
Numerical models of fast radiation-mediated shocks and planar shock breakout show that including bound-free and bound-bound opacities from solar-composition heavy elements maintains local thermal equilibrium to higher velocities and reduces breakout emission temperatures by factors of two to ten.
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
A more efficient 12C+12C rate extends carbon burning, produces less compact pre-supernova structures, and enhances s-process yields of elements heavier than Fe in supernova ejecta from 15-40 solar mass stars.
A review chapter sketching the neutrino-driven mechanism for core-collapse supernovae, the importance of nuclear physics inputs, and multi-messenger signals.
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Radiation Mediated Shock and Planar Shock Breakout in the Presence of Atomic Transition Lines
Numerical models of fast radiation-mediated shocks and planar shock breakout show that including bound-free and bound-bound opacities from solar-composition heavy elements maintains local thermal equilibrium to higher velocities and reduces breakout emission temperatures by factors of two to ten.