How magnetic fields and spin rescue dying massive stars

Simulations of a 39-solar-mass star's core collapse show that magnetic fields and rapid rotation dramatically reshape how shock waves rev­ive. Magnetic stresses extract rotational energy from the neutron star's core and channel it into polar jets, while also allowing shock revival to happen earlier than in non-magnetized cases. Rotation alone delays revival but can't sustain jets; without magnetism, even rotation fails to prevent black hole formation. This demonstrates how magnetic fields are essential for understanding which massive stars produce visible supernovae versus collapsing silently.