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We perform for the first time a 3D hydrodynamics simulation of the evolutionof the last minutes pre-collapse of the oxygen shell of a fast-rotating massivestar. This star has an initial mass of 38 M$_\odot$, a metallicity of$\sim$1/50 Z$_\odot$, an initial rotational velocity of 600 km s$^{-1}$, andexperiences chemically homogeneous evolution. It has a silicon- and oxygen-rich(Si/O) convective layer at (4.7-17)$\times 10^{8}$ cm, where oxygen-shellburning takes place. The power spectrum analysis of the turbulent velocityindicates the dominance of the large-scale mode ($\ell \sim 3$), which has alsobeen seen in non-rotating stars that have a wide Si/O layer. Spiral armstructures of density and silicon-enriched material produced by oxygen-shellburning appear in the equatorial plane of the Si/O shell. Non-axisymmetric,large-scale ($m \le 3$) modes are dominant in these structures. The spiral armstructures have not been identified in previous non-rotating 3D pre-supernovamodels. Governed by such a convection pattern, the angle-averaged specificangular momentum becomes constant in the Si/O convective layer, which is notconsidered in spherically symmetrical stellar evolution models. Such spiralarms and constant specific angular momentum might affect the ensuing explosionor implosion of the star.

A three-dimensional hydrodynamics simulation of oxygen-shell burning in the final evolution of a fast-rotating massive star