TY - JOUR
T1 - Towards an understanding of the resolution dependence of Core-Collapse Supernova simulations
AU - Nagakura, Hiroki
AU - Burrows, Adam
AU - Radice, David
AU - Vartanyan, David
N1 - Funding Information:
Grants AST-1714267 and PHY-1144374 (the latter via the Max-Planck/Princeton Center (MPPC) for Plasma Physics). DR cites partial support as a Frank and Peggy Taplin Fellow at the Institute for Advanced Study. An award of computer time was provided by the INCITE program. That research used resources of the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357. In addition, this overall research project is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This general project is also part of the ‘Three-Dimensional Simulations of Core-Collapse Supernovae’ PRAC allocation support by the National Science Foundation (under award #OAC-1809073). Moreover, access under the local award #TG-AST170045 to the resource Stampede2 in the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1548562, was crucial to the completion of this work. Finally, the authors employed computational resources provided by the TIGRESS high performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Princeton University Office of Information Technology, and acknowledge our continuing allocation at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy (DOE) under contract DE-AC03-76SF00098.
Funding Information:
The authors are grateful for ongoing contributions to this effort by Josh Dolence and Aaron Skinner. We also acknowledge Evan O’Connor regarding the equation of state, Gabriel Martínez-Pinedo concerning electron capture on heavy nuclei, Tug Sukhbold and Stan Woosley for providing details concerning the initial models, Todd Thompson regarding inelastic scattering, and Andrina Nicola for help in computing the turbulent spectrum. We acknowledge support from the U.S. Department of Energy Office of Science and the Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program and Grant DE-SC0018297 (subaward 00009650). In addition, we gratefully acknowledge support from the U.S. NSF under
Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
PY - 2019/12/1
Y1 - 2019/12/1
N2 - Using our new state-of-the-art core-collapse supernova (CCSN) code FORNAX, we explore the dependence upon spatial resolution of the outcome and character of three-dimensional (3D) supernova simulations. For the same 19 M☉ progenitor star, energy and radial binning, neutrino microphysics, and nuclear equation of state, changing only the number of angular bins in the θ and φ directions, we witness that our lowest resolution 3D simulation does not explode. However, when jumping progressively up in resolution by factors of two in each angular direction on our spherical-polar grid, models then explode, and explode slightly more vigorously with increasing resolution. This suggests that there can be a qualitative dependence of the outcome of 3D CCSN simulations upon spatial resolution. The critical aspect of higher spatial resolution is the adequate capturing of the physics of neutrino-driven turbulence, in particular its Reynolds stress. The greater numerical viscosity of lower resolution simulations results in greater drag on the turbulent eddies that embody turbulent stress, and, hence, in a diminution of their vigor. Turbulent stress not only pushes the temporarily stalled shock further out, but bootstraps a concomitant increase in the deposited neutrino power. Both effects together lie at the core of the resolution dependence we observe.
AB - Using our new state-of-the-art core-collapse supernova (CCSN) code FORNAX, we explore the dependence upon spatial resolution of the outcome and character of three-dimensional (3D) supernova simulations. For the same 19 M☉ progenitor star, energy and radial binning, neutrino microphysics, and nuclear equation of state, changing only the number of angular bins in the θ and φ directions, we witness that our lowest resolution 3D simulation does not explode. However, when jumping progressively up in resolution by factors of two in each angular direction on our spherical-polar grid, models then explode, and explode slightly more vigorously with increasing resolution. This suggests that there can be a qualitative dependence of the outcome of 3D CCSN simulations upon spatial resolution. The critical aspect of higher spatial resolution is the adequate capturing of the physics of neutrino-driven turbulence, in particular its Reynolds stress. The greater numerical viscosity of lower resolution simulations results in greater drag on the turbulent eddies that embody turbulent stress, and, hence, in a diminution of their vigor. Turbulent stress not only pushes the temporarily stalled shock further out, but bootstraps a concomitant increase in the deposited neutrino power. Both effects together lie at the core of the resolution dependence we observe.
KW - Supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=85077267801&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85077267801&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz2730
DO - 10.1093/mnras/stz2730
M3 - Article
AN - SCOPUS:85077267801
SN - 0035-8711
VL - 490
SP - 4622
EP - 4637
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -