Non-axisymmetric features are found in the core collapse of a rapidly rotating massive star , which might have important implications for magnetic field amplification and production of a bipolar outflow that can explode the star , as well as for r -process nucleosynthesis and natal kicks .
The collapse of an evolved rapidly rotating M _ { \mathrm { ZAMS } } = 54 M _ { \odot } star is followed in three-dimensional hydrodynamic simulations using the flash code with neutrino leakage .
A rotating proto-neutron star ( PNS ) forms with a non-zero linear velocity .
This can contribute to the natal kick of the remnant compact object .
The PNS is surrounded by a turbulent medium , where high shearing is likely to amplify magnetic fields , which in turn can drive a bipolar outflow .
Neutron-rich material in the PNS vicinity might induce strong r -process nucleosynthesis .
The rapidly rotating PNS possesses a rotational energy of E _ { \mathrm { rot } } \ga 10 ^ { 52 } ~ { } \mathrm { erg } .
Magnetar formation proceeding in a similar fashion will be able to deposit a portion of this energy later on in the SN ejecta through a spin down mechanism .
These processes can be important for rare supernovae generated by rapidly rotating progenitors , even though a complete explosion is not simulated in the present study .

Key words : stars : massive — stars : rotation — supernovae : general