Three dimensional magnetorotational core-collapse supernova explosions of a 39 solar mass progenitor star

Understand

We perform three-dimensional simulations of magnetorotational supernovae using a $39\,M_{\odot}$ progenitor star with two different initial magnetic field strengths of $10^{10}$ G and $10^{12}$ G in the core.

• Both models rapidly undergo shock revival and their explosion energies asymptote within a few hundred milliseconds to values of $\gtrsim 2\times10^{51}$ erg after conservatively correcting for the binding energy of the envelope.
• Magnetically collimated, non-relativistic jets form in both models, though the jets are subject to non-axisymmetric instabilities.
• The jets do not appear crucial for driving the explosion, as they only emerge once the shock has already expanded considerably.