期刊
ASTROPHYSICAL JOURNAL
卷 808, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/0004-637X/808/1/70
关键词
hydrodynamics; neutrinos; supernovae: general
资金
- NSF [AST-1212170, PHY-1404569, PHY-1151197, PHY-1212460, OCI-0905046]
- NSERC [RGPIN 418680-2012]
- Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory
- Sloan Research Foundation
- Sherman Fairchild Foundation
- NASA [PF2-130099, PF3-140114, NAS8-03060]
- Chandra X-ray center
- NSF MRI award [PHY-0960291]
- NSF PRAC award [ACI-1440083]
- Office of Science of US Department of Energy [DE-AC02-05CH11231]
- Direct For Mathematical & Physical Scien
- Division Of Physics [1212401, 1151197, 1212460] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1205732, 1212170] Funding Source: National Science Foundation
- Office of Advanced Cyberinfrastructure (OAC)
- Direct For Computer & Info Scie & Enginr [1440083, 1440050] Funding Source: National Science Foundation
- Office of Advanced Cyberinfrastructure (OAC)
- Direct For Computer & Info Scie & Enginr [0905046] Funding Source: National Science Foundation
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-circle dot 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), and (3) SASI-dominated evolution. This confirms previous 3D results of Hanke et al. and Couch & Connor. We carry out simulations with resolutions differing by up to a factor of similar to 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) proportional to l(-1) in the inertial range,while theory and local simulations argue for E(l) proportional to 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.
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