EPJ Web Conf.
Volume 260, 2022The 16th International Symposium on Nuclei in the Cosmos (NIC-XVI)
|Number of page(s)||3|
|Published online||24 February 2022|
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: email@example.com
Published online: 24 February 2022
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.
© The Authors, published by EDP Sciences, 2022
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