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Free keywords:
Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
Abstract:
We perform for the first time a 3D hydrodynamics simulation of the evolution
of the last minutes pre-collapse of the oxygen shell of a fast-rotating massive
star. 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}$, and
experiences chemically homogeneous evolution. It has a silicon- and oxygen-rich
(Si/O) convective layer at (4.7-17)$\times 10^{8}$ cm, where oxygen-shell
burning takes place. The power spectrum analysis of the turbulent velocity
indicates the dominance of the large-scale mode ($\ell \sim 3$), which has also
been seen in non-rotating stars that have a wide Si/O layer. Spiral arm
structures of density and silicon-enriched material produced by oxygen-shell
burning 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 arm
structures have not been identified in previous non-rotating 3D pre-supernova
models. Governed by such a convection pattern, the angle-averaged specific
angular momentum becomes constant in the Si/O convective layer, which is not
considered in spherically symmetrical stellar evolution models. Such spiral
arms and constant specific angular momentum might affect the ensuing explosion
or implosion of the star.
