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

Abdikamalov, E., Ott, C. D., Radice, D., Roberts, L. F., Haas, R., Reisswig, C., et al. (2015). Neutrino-driven Turbulent Convection and Standing Accretion Shock Instability in Three-Dimensional Core-Collapse Supernovae. The Astrophysical Journal, 808(1): 70. doi:10.1088/0004-637X/808/1/70.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-0025-B8CF-E Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-0028-5906-6
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 Urheber:
Abdikamalov, E.1, Autor
Ott, C. D.2, Autor              
Radice, D., Autor
Roberts, L. F., Autor
Haas, R.3, Autor              
Reisswig, C.4, Autor              
Moesta, P.4, Autor              
Klion, H., Autor
Schnetter, E.2, Autor              
Affiliations:
1TAPIR, Caltech, escidoc:persistent22              
2Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, escidoc:159882              
3Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              
4Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:24013              

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Schlagwörter: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR
 Zusammenfassung: 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 $27$-$M_\odot$ 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 $\sim$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 $E(\ell)$ develops in the heating layer. Like other 3D studies, we find $E(\ell) \propto \ell^{-1}$ in the "inertial range," while theory and local simulations argue for $E(\ell) \propto \ell^{-5/3}$. 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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 Datum: 2014-09-242015
 Publikationsstatus: Im Druck publiziert
 Seiten: 22 pages, 14 figures. Submitted to The Astrophysical Journal
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Identifikatoren: arXiv: 1409.7078
DOI: 10.1088/0004-637X/808/1/70
 Art des Abschluß: -

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Titel: The Astrophysical Journal
Genre der Quelle: Zeitschrift
 Urheber:
Affiliations:
Ort, Verlag, Ausgabe: Chicago, IL : University of Chicago Press for the American Astronomical Society
Seiten: - Band / Heft: 808 (1) Artikelnummer: 70 Start- / Endseite: - Identifikator: ISSN: 0004-637X
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/954922828215_3