CaltechAUTHORS
  A Caltech Library Service

Neutrino-driven Turbulent Convection and Standing Accretion Shock Instability in Three-Dimensional Core-Collapse Supernovae

Abdikamalov, Ernazar and Ott, Christian D. and Radice, David and Roberts, Luke F. and Haas, Roland and Reisswig, Christian and Mösta, Philipp and Klion, Hannah and Schnetter, Erik (2015) Neutrino-driven Turbulent Convection and Standing Accretion Shock Instability in Three-Dimensional Core-Collapse Supernovae. Astrophysical Journal, 808 (1). Art. No. 70. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20141217-093048536

[img] PDF - Published Version
See Usage Policy.

2840Kb
[img]
Preview
PDF - Submitted Version
See Usage Policy.

3546Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20141217-093048536

Abstract

We conduct a series of numerical experiments into the nature of three-dimensional (3D) hydrodynamics in the postbounce stalled-shock phase of core-collapse supernovae using 3D general-relativistic hydrodynamic simulations of a 27-M⊙ progenitor star with a neutrino leakage/heating scheme. We vary the strength of neutrino heating and find three cases of 3D dynamics: (1) neutrino-driven convection, (2) initially neutrino-driven convection and subsequent development of the standing accretion shock instability (SASI), (3) SASI dominated evolution. This confirms previous 3D results of Hanke et al. 2013, ApJ 770, 66 and Couch & Connor 2014, ApJ 785, 123. We carry out simulations with resolutions differing by up to a factor of ∼4 and demonstrate that low resolution is artificially favorable for explosion in the 3D convection-dominated case, since it decreases the efficiency of energy transport to small scales. Low resolution results in higher radial convective fluxes of energy and enthalpy, more fully buoyant mass, and stronger neutrino heating. In the SASI-dominated case, lower resolution damps SASI oscillations. In the convection-dominated case, a quasi-stationary angular kinetic energy spectrum E(ℓ) develops in the heating layer. Like other 3D studies, we find E(ℓ)∝ℓ−1 in the "inertial range," while theory and local simulations argue for E(ℓ)∝ℓ−5/3. We argue that current 3D simulations do not resolve the inertial range of turbulence and are affected by numerical viscosity up to the energy containing scale, creating a "bottleneck" that prevents an efficient turbulent cascade.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1409.7078arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/808/1/70DOIArticle
http://iopscience.iop.org/0004-637X/808/1/70/PublisherArticle
ORCID:
AuthorORCID
Ott, Christian D.0000-0003-4993-2055
Roberts, Luke F.0000-0001-7364-7946
Additional Information:© 2015 American Astronomical Society. Received 2014 September 24; accepted 2015 June 3; published 2015 July 17. We thank Sean Couch, Peter Goldreich, and Mike Norman for helpful discussions on turbulence and Thierry Foglizzo for help with interpreting the behavior of SASI in our simulations. We furthermore acknowledge helpful discussions with Adam Burrows, Joshua Dolence, Steve Drasco, Rodrigo Fernandez, Sarah Gossan, Thomas Janka, Bernhard Müller, Jeremiah Murphy, Evan O’Connor, Sherwood Richers, and other members of our Simulating eXtreme Spacetimes (SXS) collaboration (http://www.black-holes.org). This research is partially supported by NSF grant nos. AST-1212170, PHY-1404569, PHY-1151197, PHY-1212460, and OCI-0905046,by NSERC grant RGPIN 418680-2012, by a grant from the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory, by the Sloan Research Foundation, and by the Sherman Fairchild Foundation. CR and LR acknowledge support by NASA through Einstein Postdoctoral Fellowship grant numbers PF2-130099 and PF3-140114, respectively, awarded by the Chandra X-ray center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. The simulations were performed on the Caltech compute cluster “Zwicky”(NSF MRI award No. PHY-0960291), on supercomputers of the NSF XSEDE network under computer time allocation TG-PHY100033, on the NSF/NCSA Blue Waters system under NSF PRAC award ACI-1440083, on machines of the Louisiana Optical Network Initiative, and at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy under contract DE-AC02-05CH11231. The multi-dimensional visualizations were generated with the open-source VisIt visualization package (https://wci.llnl.gov/codes/visit/). All other figures were generated with the Python-based matplotlib package (Hunter 2007, http://matplotlib.org/).
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-1212170
NSFPHY-1404569
NSFPHY-1151197
NSFPHY-1212460
NSFOCI-0905046
Los Alamos National LaboratoryUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN 418680-2012
Alfred P. Sloan FoundationUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NASA Einstein Postdoctoral FellowshipPF2-130099
NASA Einstein Postdoctoral FellowshipPF3-140114
NASANAS8-03060
NSFPHY-0960291
Department of Energy (DOE)DE-AC02-05CH11231
Non-Subject Keywords:hydrodynamics, neutrinos, Stars: supernovae: general
Issue or Number:1
Record Number:CaltechAUTHORS:20141217-093048536
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20141217-093048536
Official Citation:Neutrino-driven Turbulent Convection and Standing Accretion Shock Instability in Three-dimensional Core-collapse Supernovae Ernazar Abdikamalov et al. 2015 ApJ 808 70
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:52941
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:17 Dec 2014 17:47
Last Modified:03 Oct 2019 07:45

Repository Staff Only: item control page