We present the results of a numerical magnetohydrodynamic simulation that demonstrates a mechanism by which magnetic fields tap the rotational energy of a stellar core and expel the envelope. Our numerical setup, designed to focus on the basic physics of the outflow mechanism, consists of a solid, gravitating sphere, which may represent the compact core of a star, surrounded by an initially hydrostatic envelope of ionized gas. The core is threaded by a dipolar magnetic field that also permeates the envelope. At the start of the simulation, the core begins to rotate at 10% of the escape speed. The magnetic field is sufficiently strong to drive a magneto-rotational explosion, whereby the entire envelope is expelled, confirming the expectation of analytical models. Furthermore, the dipolar nature of the field results in an explosion that is enhanced simultaneously along the rotation axis (a jet) and along the magnetic equator. While the initial condition is simplified, the simulation approximates circumstances that may arise in astrophysical objects such as Type Ⅱ supernovae, gamma-ray bursts, and proto-planetary nebulae.
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