Three-dimensional hydrodynamics simulations of shell burning in Si/O-rich layer of pre-collapse massive stars

¹ Yukawa Institute for TheoreticalPhysics,Kyoto University, Kyoto 606-8502, Japan
² Divisionof Science, National Astronomical Observatoryof Japan, Tokyo 181-8588, Japan
³ Department of Applied Physics&Research Institute of Stellar Explosive Phenomena, Fukuoka University, Fukuoka 814-0180, Japan
⁴ Max-Planck-Institute for Gravitational Physics, D-14476 Potsdam, Germany
⁵ Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
⁶ Institute of Astrophysics, FORTH, Department of Physics, University of Crete, GR-71003 Heraklion, Greece
⁷ Argelander-Institut für Astronomie, Universität Bonn, D-53121 Bonn, Germany
⁸ Max-Planck-Institute für Radioastronomie, D-53121 Bonn, Germany

^* e-mail: yoshida@yukawa.kyoto-u.ac.jp

Published online: 24 February 2022

Abstract

We perform three-dimensional (3D)hydrodynamics simulations of shell burning in the silicon-and oxygen-rich layers in pre-collapse massive stars.Weadoptanon-rotating27 M_⊙ starhaving anextended O/Si/Ne layer and afast-rotating 38 M_⊙ star having a Si/Olayer, that has experienced chemically homogeneousevolution. Both pre-collapse stars showlarge-scale turbulent motion with a maximum Mach number of ~0.1 in the convective layers activated byneonand oxygenshellburning.The radialproflieoftheangle-averaged mass fraction distributioninO/Si/Ne layer is more homogeneous in the 3D simulation compared to the 1D evolution for the 27 M_⊙ star. The angle-averaged specific angular momentum in the Si/O layer of the fast-rotating 38 M_⊙ star tends to become roughly constant in the convective layer of the 3D simulation, which is not considered in the 1D evolution.