TY - JOUR
T1 - Turbulence in core-collapse supernovae
AU - Radice, David
AU - Abdikamalov, Ernazar
AU - Ott, Christian D.
AU - Mösta, Philipp
AU - Couch, Sean M.
AU - Roberts, Luke F.
N1 - Funding Information:
The authors acknowledge Adam Burrows, Jérôme Guilet, Roland Haas, Thierry Foglizzo, Bernhard Müller, Jeremiah WMurphy, and Evan O’Connor for insightful discussion on the explosion mechanism of core-collapse supernovae, and the anonymous referee for valuable suggestions that improved the quality of this manuscript. DR gratefully acknowledges support from the Schmidt Fellowship, the Sherman Fairchild Foundation and the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). CDO is partially supported by NSF grant CAREER PHY-1151197. SMC is supported by the US Department of Energy, Office of Science, Office of Nuclear Physics, under Award Numbers DE-SC0015904 and DESC0017955 and the Chandra x-ray Observatory under grant TM7-18005X. Work presented in this review benefitted from computer time allocations at NSF/NCSA Blue Waters (PRAC ACI-1440083), at the National Energy Research Scientific Computing Center (project m152), a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, and on the Texas Advanced Computing Center Stampede cluster under NSF XSEDE allocation TG-PHY100033. Simulations described herein where completed with computer time provided by the Innovative and Novel Computational Impact on Theory and Experiment (INCITE) program. This research used resources of the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357.
Funding Information:
DR gratefully acknowledges support from the Schmidt Fellowship, the Sherman Fairchild Foundation and the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). CDO is partially supported by NSF grant CAREER PHY-1151197. SMC is supported by the US Department of Energy, Office of Science, Office of Nuclear Physics, under Award Numbers DE-SC0015904 and DESC0017955 and the Chandra x-ray Observatory under grant TM7-18005X.
Publisher Copyright:
© 2018 IOP Publishing Ltd.
PY - 2018/4/9
Y1 - 2018/4/9
N2 - Multidimensional simulations show that non-radial, turbulent, fluid motion is a fundamental component of the core-collapse supernova explosion mechanism. Neutrino-driven convection, the standing accretion shock instability, and relic-perturbations from advanced nuclear burning stages can all impact the outcome of core collapse in a qualitative and quantitative way. Here, we review the current understanding of these phenomena and their role in the explosion of massive stars. We also discuss the role of protoneutron star convection and of magnetic fields in the context of the delayed neutrino mechanism.
AB - Multidimensional simulations show that non-radial, turbulent, fluid motion is a fundamental component of the core-collapse supernova explosion mechanism. Neutrino-driven convection, the standing accretion shock instability, and relic-perturbations from advanced nuclear burning stages can all impact the outcome of core collapse in a qualitative and quantitative way. Here, we review the current understanding of these phenomena and their role in the explosion of massive stars. We also discuss the role of protoneutron star convection and of magnetic fields in the context of the delayed neutrino mechanism.
KW - astrophysical turbulence
KW - methods: numerical
KW - supernovae
UR - http://www.scopus.com/inward/record.url?scp=85046656428&partnerID=8YFLogxK
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U2 - 10.1088/1361-6471/aab872
DO - 10.1088/1361-6471/aab872
M3 - Review article
AN - SCOPUS:85046656428
SN - 0954-3899
VL - 45
JO - Journal of Physics G: Nuclear and Particle Physics
JF - Journal of Physics G: Nuclear and Particle Physics
IS - 5
M1 - 053003
ER -