dc.contributor.author |
Abdikamalov, Ernazar
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dc.contributor.author |
Ott, Christian D.
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|
dc.contributor.author |
Radice, David
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dc.contributor.author |
Roberts, Luke F.
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dc.contributor.author |
Haas, Roland
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dc.contributor.author |
Reisswig, Christian
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dc.contributor.author |
Mosta, Philipp
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dc.contributor.author |
Klion, Hannan
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dc.contributor.author |
Schnetter, Erik
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dc.date.accessioned |
2015-12-22T08:06:35Z |
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dc.date.available |
2015-12-22T08:06:35Z |
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dc.date.issued |
2015-06-04 |
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dc.identifier.citation |
Abdikamalov Ernazar, Ott Christian D., Radice David, Roberts Luke F., Haas Roland, Reisswig Christian, Mosta Philipp, Klion Hannan, Schnetter Erik; 2015; Neutrino-driven turbulent convection and standing accretion shock instability in three-dimensional core-collapse supernovae; http://arxiv.org/find/all/1/all:+abdikamalov/0/1/0/all/0/1 |
ru_RU |
dc.identifier.uri |
http://nur.nu.edu.kz/handle/123456789/939 |
|
dc.description.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 nd 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 con rms previous 3D results of Hanke
et al. (2013), ApJ 770:66 and Couch & Connor (2014), ApJ 785:123. We carry out simulations with resolutions di ering by up to a factor of 4 and demonstrate that low resolution is arti cially favorable for explosion in the 3D convection-dominated case, since it decreases the e ciency of energy transport to small scales. Low resolution results in higher radial convective uxes 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(`) develops in the heating layer. Like other 3D studies, we nd E(`) / `1 in the \inertial range," while theory and local simulations argue for E(`) / `5=3. We argue that current 3D simulations do not resolve the inertial range of turbulence and are a ected by numerical viscosity up to the energy containing scale, creating a \bottleneck" that prevents an e cient turbulent cascade |
ru_RU |
dc.language.iso |
en |
ru_RU |
dc.subject |
Research Subject Categories::NATURAL SCIENCES::Physics |
ru_RU |
dc.subject |
hydrodynamics |
ru_RU |
dc.subject |
neutrinos |
ru_RU |
dc.subject |
supernovae |
ru_RU |
dc.title |
Neutrino-driven turbulent convection and standing accretion shock instability in three-dimensional core-collapse supernovae |
ru_RU |
dc.type |
Article |
ru_RU |