期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 506, 期 1, 页码 L20-L25出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnrasl/slab067
关键词
convection; hydrodynamics; stars: massive; stars: rotation
资金
- Japan Society for the Promotion of Science (JSPS) KAKENHI [JP17H05206, JP17K14306, JP17H01130, JP17H06364, JP18H01212, JP20H05249]
- Central Research Institute of Explosive Stellar Phenomena (REISEP) of Fukuoka University [207002]
- Stavros Niarchos Foundation (SNF)
- Hellenic Foundation for Research and Innovation [01431]
A 3D hydrodynamics simulation was conducted for the evolution of the oxygen shell of a fast-rotating massive star, revealing the presence of spiral arm structures in the equatorial plane of the Si/O shell, which might affect the explosion or implosion of the star.
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-circle dot, a metallicity of similar to 1/50 Z(circle dot), 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) x 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 (l similar to 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 <= 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.
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