General-Relativistic Three-Dimensional Multi-group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae
Abstract
We report on a set of long-term general-relativistic three-dimensional (3D) multi-group (energy-dependent) neutrino radiation-hydrodynamics simulations of core-collapse supernovae. We employ a full 3D two-moment scheme with the local M1 closure, three neutrino species, and 12 energy groups per species. With this, we follow the post-core-bounce evolution of the core of a nonrotating 27-M⊙ progenitor in full unconstrained 3D and in octant symmetry for ≳380 ms. We find the development of an asymmetric runaway explosion in our unconstrained simulation. We test the resolution dependence of our results and, in agreement with previous work, find that low resolution artificially aids explosion and leads to an earlier runaway expansion of the shock. At low resolution, the octant and full 3D dynamics are qualitatively very similar, but at high resolution, only the full 3D simulation exhibits the onset of explosion.
Additional Information
© 2016 The American Astronomical Society. Received 2016 April 26; revised 2016 July 26; accepted 2016 July 26; published 2016 October 28. The authors would like to thank E Abdikamalov, WD Arnett, A Burrows, S Couch, F Foucart, K Kiuchi, J Lattimer, C Meakin, P Mösta, D Radice, Y Sekiguchi, and M Shibata for their discussions. CDO wishes to thank the Yukawa Institute for Theoretical Physics for their hospitality during the completion of this work. Support for LR during this work was provided by NASA through an Einstein Postdoctoral Fellowship grant, PF3-140114, awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This research was partially supported by NSF grants AST-1212170, CAREER PHY-1151197, PHY-1404569, AST-1333520, and OCI-0905046; the Sherman Fairchild Foundation; and the International Research Unit of Advanced Future Studies, Kyoto University. Support for EO during 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. This research was supported in part by the Perimeter Institute for Theoretical Physics. Research at the Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science, and Economic Development and by the Province of Ontario through the Ministry of Research and Innovation. The simulations were carried out on the NSF XSEDE network (allocation TG-PHY100033) and on NSF/NCSA Blue Waters (PRAC award ACI-1440083). This paper has been assigned Yukawa Institute for Theoretical Physics report number YITP-16-54.Attached Files
Published - Roberts_2016_ApJ_831_98.pdf
Submitted - 1604.07848v1.pdf
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Additional details
- Eprint ID
- 71569
- Resolver ID
- CaltechAUTHORS:20161028-100923991
- PF3-140114
- NASA Einstein Postdoctoral Fellowship
- NAS8-03060
- NASA
- AST-1212170
- NSF
- PHY-1151197
- NSF
- PHY-1404569
- NSF
- AST-1333520
- NSF
- OCI-0905046
- NSF
- Sherman Fairchild Foundation
- Kyoto University
- 51344.001-A
- NASA Hubble Fellowship
- NAS 5-26555
- NASA
- Perimeter Institute for Theoretical Physics
- Department of Innovation, Science, and Economic Development (Canada)
- Ontario Ministry of Research and Innovation
- TG-PHY100033
- NSF
- ACI-1440083
- NSF
- Created
-
2016-10-28Created from EPrint's datestamp field
- Updated
-
2023-03-16Created from EPrint's last_modified field
- Caltech groups
- TAPIR, Walter Burke Institute for Theoretical Physics