TY - JOUR
T1 - 2D numerical study for magnetic field dependence of neutrino-driven core-collapse supernova models
AU - Matsumoto, J.
AU - Takiwaki, T.
AU - Kotake, K.
AU - Asahina, Y.
AU - Takahashi, H. R.
N1 - Funding Information:
We thank K. Nakamura, M. Bugli, Y. Masada, Y. Matsumoto, K. Tomisaka, and H.-Th. Janka for useful and stimulating discussions. Numerical computations were carried out on Cray XC50 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan and on Cray XC40 at YITP in Kyoto University. This work was supported by Research Institute of Stellar Explosive Phenomena at Fukuoka University and the associated project (No. 207002), and also by JSPS KAKENHI Grant Number (JP17K14260, JP17H05206, JP17K14306, JP17H01130, JP17H06364, JP18H01212, JP18K13591, JP19K23443, JP20K14473, JP20K11851, JP20H01941, and JP20H00156). This research was also supported by MEXT as 'Program for Promoting researches on the Supercomputer Fugaku' (Towards a unified view of the Universe: from large-scale structures to planets) and Joint Institute for Computational Fundamental Science (JICFuS).
Publisher Copyright:
© The Author(s) 2020.
PY - 2020/12/1
Y1 - 2020/12/1
N2 - We study the effects of the magnetic field on the dynamics of non-rotating stellar cores by performing 2D, magnetohydrodynamic (MHD) simulations. To this end, we have updated our neutrino-radiation-hydrodynamics supernova code to include MHD employing a divergence cleaning method with both careful treatments of finite volume and area reconstructions. By changing the initial strength of the magnetic field, the evolution of 15.0, 18.4, and 27.0 M☉ pre-supernova progenitors is investigated. An intriguing finding in our study is that the neutrino-driven explosion occurs regardless of the strength of the initial magnetic field. For the 2D models presented in this work, the neutrino heating is the main driver for the explosion, whereas the magnetic field secondary contributes to the pre-explosion dynamics. Our results show that the strong magnetic field weakens the growth of the neutrino-driven turbulence in the small scale compared to the weak magnetic field. This results in the slower increase of the turbulent kinetic energy in the post-shock region, leading to the slightly delayed onset of the shock revival for models with the stronger initial magnetic field.
AB - We study the effects of the magnetic field on the dynamics of non-rotating stellar cores by performing 2D, magnetohydrodynamic (MHD) simulations. To this end, we have updated our neutrino-radiation-hydrodynamics supernova code to include MHD employing a divergence cleaning method with both careful treatments of finite volume and area reconstructions. By changing the initial strength of the magnetic field, the evolution of 15.0, 18.4, and 27.0 M☉ pre-supernova progenitors is investigated. An intriguing finding in our study is that the neutrino-driven explosion occurs regardless of the strength of the initial magnetic field. For the 2D models presented in this work, the neutrino heating is the main driver for the explosion, whereas the magnetic field secondary contributes to the pre-explosion dynamics. Our results show that the strong magnetic field weakens the growth of the neutrino-driven turbulence in the small scale compared to the weak magnetic field. This results in the slower increase of the turbulent kinetic energy in the post-shock region, leading to the slightly delayed onset of the shock revival for models with the stronger initial magnetic field.
KW - Stars: magnetic field
KW - Stars: massive
KW - Supernovae: general
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U2 - 10.1093/mnras/staa3095
DO - 10.1093/mnras/staa3095
M3 - Article
AN - SCOPUS:85097159034
SN - 0035-8711
VL - 499
SP - 4174
EP - 4194
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -