Global comparison of core-collapse supernova simulations in spherical symmetry

Evan O'Connor; Robert Bollig; Adam Burrows; Sean Couch; Tobias Fischer; Hans Thomas Janka; Kei Kotake; Eric J. Lentz; Matthias Liebendörfer; O. E.Bronson Messer; Anthony Mezzacappa; Tomoya Takiwaki; David Vartanyan

doi:10.1088/1361-6471/aadeae

Global comparison of core-collapse supernova simulations in spherical symmetry

Evan O'Connor, Robert Bollig, Adam Burrows, Sean Couch, Tobias Fischer, Hans Thomas Janka, Kei Kotake, Eric J. Lentz, Matthias Liebendörfer, O. E.Bronson Messer, Anthony Mezzacappa, Tomoya Takiwaki, David Vartanyan

National Center for Computational Scienc

Research output: Contribution to journal › Article › peer-review

117 Scopus citations

Abstract

We present a comparison between several simulation codes designed to study the core-collapse supernova mechanism. We pay close attention to controlling the initial conditions and input physics in order to ensure a meaningful and informative comparison. Our goal is three-fold. First, we aim to demonstrate the current level of agreement between various groups studying the core-collapse supernova central engine. Second, we desire to form a strong basis for future simulation codes and methods to compare to. Lastly, we want this work to be a stepping stone for future work exploring more complex simulations of core-collapse supernovae, i.e., simulations in multiple dimensions and simulations with modern neutrino and nuclear physics. We compare the early (first ∼500 ms after core bounce) spherically-symmetric evolution of a 20 M progenitor star from six different core-collapse supernovae codes: 3DnSNe-IDSA, AGILE-BOLTZTRAN, FLASH, Fornax, GR1D, and PROMETHEUS-VERTEX. Given the diversity of neutrino transport and hydrodynamic methods employed, we find excellent agreement in many critical quantities, including the shock radius evolution and the amount of neutrino heating. Our results provide an excellent starting point from which to extend this comparison to higher dimensions and compare the development of hydrodynamic instabilities that are crucial to the supernova explosion mechanism, such as turbulence and convection.

Original language	English
Article number	104001
Journal	Journal of Physics G: Nuclear and Particle Physics
Volume	45
Issue number	10
DOIs	https://doi.org/10.1088/1361-6471/aadeae
State	Published - Sep 14 2018

Funding

Fornax: AB and DV employed computational resources for this study 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. AB acknowledges support under US NSF Grant AST-1714267 and the Max Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1144374), and by the DOE SciDAC4 Grant DE-SC0018297 (subaward 00009650). 3DnSNe-IDSA: KK and TT acknowledge support by the JSPS KAKENHI Grant Numbers (JP15H00789, JP15H01039, JP17H01130, JP17H06364, JP17K14306, JP17H05206, and JP18H01212), and by the Central Research Institute of Fukuoka University (Nos.171042, 177103), and by JICFuS which chose the code development of 3DnSNe-IDSA as a priority issue to be tackled by using the Post ‘K’ Computer. Prometheus-Vertex: At Garching, this work was supported by the European Research Council through grant ERC AdG 341157-COCO2CASA, and by the Deutsche For-schungsgemeinschaft (DFG) through the Cluster of Excellence ‘Universe’ (EXC 153) and Sonderforschungsbereich ‘Neutrinos and Dark Matter in Astro-and Particle Physics’ (SFB 1258). Computational resources by the Max Planck Computing and Data Facility (MPCDF) are acknowledged. FLASH & GR1D: EO acknowledges that partial support for this work was provided by NASA through Hubble Fellowship grant #51344.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. SMC is supported by the US Department of Energy, Office of Science, Office of Nuclear Physics, under Award Numbers DE-SC0015904 and DE-SC0017955 and the Chandra x-ray Observatory under grant TM7-18005X. FLASH & GR1D computations were performed on resources provided by the Swedish National Infrastructure for Computing (SNIC) at the PDC Center for High Performance Computing (PDC). Agile-Boltztran: TF acknowledges support by the Polish National Science Center (NCN) under grant number UMO-2016/23/B/ST2/00720. This work was supported by the COST Actions CA16117 ‘ChETEC’ and CA16214 ‘PHAROS’. AM acknowledges support from the National Science Foundation (NSF GP 1505933). The Agile-Boltztran supernova simulations were performed at the Wroclaw Center for Supercomputing and Networking (WCSS).

Funders	Funder number
Deutsche For-schungsgemeinschaft	EXC 153, SFB 1258
JICFuS
Max Planck/Princeton Center
Office of Nuclear Physics	DE-SC0015904, TM7-18005X, DE-SC0017955
Polish National Science Center
Princeton Institute for Computational Science and Engineering
Princeton University Office of Information Technology
US Department of Energy
National Science Foundation	1804048, PHY-1144374, AST-1714267, GP 1505933
U.S. Department of Energy	DE-SC0018297
National Aeronautics and Space Administration	51344.001-A
Office of Science
Seventh Framework Programme	341157
Space Telescope Science Institute	NAS 5-26555
European Research Council
European Cooperation in Science and Technology	CA16214
Japan Society for the Promotion of Science	JP17H05206, 17H01130, JP15H00789, 15KK0173, 17K14306, JP17H06364, JP18H01212, JP15H01039
Narodowe Centrum Nauki	UMO-2016/23/B/ST2/00720
Central Research Institute, Fukuoka University	171042, 177103

Keywords

code comparison
core-collapse supernovae
neutrino transport
neutron stars

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10.1088/1361-6471/aadeae

Cite this

O'Connor, E., Bollig, R., Burrows, A., Couch, S., Fischer, T., Janka, H. T., Kotake, K., Lentz, E. J., Liebendörfer, M., Messer, O. E. B., Mezzacappa, A., Takiwaki, T., & Vartanyan, D. (2018). Global comparison of core-collapse supernova simulations in spherical symmetry. Journal of Physics G: Nuclear and Particle Physics, 45(10), Article 104001. https://doi.org/10.1088/1361-6471/aadeae

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AU - Kotake, Kei

AU - Lentz, Eric J.

AU - Liebendörfer, Matthias

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AB - We present a comparison between several simulation codes designed to study the core-collapse supernova mechanism. We pay close attention to controlling the initial conditions and input physics in order to ensure a meaningful and informative comparison. Our goal is three-fold. First, we aim to demonstrate the current level of agreement between various groups studying the core-collapse supernova central engine. Second, we desire to form a strong basis for future simulation codes and methods to compare to. Lastly, we want this work to be a stepping stone for future work exploring more complex simulations of core-collapse supernovae, i.e., simulations in multiple dimensions and simulations with modern neutrino and nuclear physics. We compare the early (first ∼500 ms after core bounce) spherically-symmetric evolution of a 20 M progenitor star from six different core-collapse supernovae codes: 3DnSNe-IDSA, AGILE-BOLTZTRAN, FLASH, Fornax, GR1D, and PROMETHEUS-VERTEX. Given the diversity of neutrino transport and hydrodynamic methods employed, we find excellent agreement in many critical quantities, including the shock radius evolution and the amount of neutrino heating. Our results provide an excellent starting point from which to extend this comparison to higher dimensions and compare the development of hydrodynamic instabilities that are crucial to the supernova explosion mechanism, such as turbulence and convection.

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Global comparison of core-collapse supernova simulations in spherical symmetry

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