Abstract
Nuclear shell burning in the final stages of the lives of massive stars is accompanied by strong turbulent convection. The resulting fluctuations aid supernova explosion by amplifying the non-radial flow in the post-shock region. In this work, we investigate the physical mechanism behind this amplification using a linear perturbation theory. We model the shock wave as a one-dimensional planar discontinuity and consider its interaction with vorticity and entropy perturbations in the upstream flow. We find that, as the perturbations cross the shock, their total turbulent kinetic energy is amplified by a factor of ~2, while the average linear size of turbulent eddies decreases by about the same factor. These values are not sensitive to the parameters of the upstream turbulence and the nuclear dissociation efficiency at the shock. Finally, we discuss the implication of our results for the supernova explosion mechanism. We show that the upstream perturbations can decrease the critical neutrino luminosity for producing explosion by several per cent.
| Original language | English |
|---|---|
| Pages (from-to) | 3864-3876 |
| Number of pages | 13 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 461 |
| Issue number | 4 |
| DOIs | |
| Publication status | Published - Oct 1 2016 |
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Keywords
- General
- Hydrodynamics-shock waves-turbulence-supernovae
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Shock-turbulence interaction in core-collapse supernovae. / Abdikamalov, Ernazar; Zhaksylykov, Azamat; Radice, David; Berdibek, Shapagat.
In: Monthly Notices of the Royal Astronomical Society, Vol. 461, No. 4, 01.10.2016, p. 3864-3876.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Shock-turbulence interaction in core-collapse supernovae
AU - Abdikamalov, Ernazar
AU - Zhaksylykov, Azamat
AU - Radice, David
AU - Berdibek, Shapagat
PY - 2016/10/1
Y1 - 2016/10/1
N2 - Nuclear shell burning in the final stages of the lives of massive stars is accompanied by strong turbulent convection. The resulting fluctuations aid supernova explosion by amplifying the non-radial flow in the post-shock region. In this work, we investigate the physical mechanism behind this amplification using a linear perturbation theory. We model the shock wave as a one-dimensional planar discontinuity and consider its interaction with vorticity and entropy perturbations in the upstream flow. We find that, as the perturbations cross the shock, their total turbulent kinetic energy is amplified by a factor of ~2, while the average linear size of turbulent eddies decreases by about the same factor. These values are not sensitive to the parameters of the upstream turbulence and the nuclear dissociation efficiency at the shock. Finally, we discuss the implication of our results for the supernova explosion mechanism. We show that the upstream perturbations can decrease the critical neutrino luminosity for producing explosion by several per cent.
AB - Nuclear shell burning in the final stages of the lives of massive stars is accompanied by strong turbulent convection. The resulting fluctuations aid supernova explosion by amplifying the non-radial flow in the post-shock region. In this work, we investigate the physical mechanism behind this amplification using a linear perturbation theory. We model the shock wave as a one-dimensional planar discontinuity and consider its interaction with vorticity and entropy perturbations in the upstream flow. We find that, as the perturbations cross the shock, their total turbulent kinetic energy is amplified by a factor of ~2, while the average linear size of turbulent eddies decreases by about the same factor. These values are not sensitive to the parameters of the upstream turbulence and the nuclear dissociation efficiency at the shock. Finally, we discuss the implication of our results for the supernova explosion mechanism. We show that the upstream perturbations can decrease the critical neutrino luminosity for producing explosion by several per cent.
KW - General
KW - Hydrodynamics-shock waves-turbulence-supernovae
UR - http://www.scopus.com/inward/record.url?scp=84988600874&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84988600874&partnerID=8YFLogxK
U2 - 10.1093/mnras/stw1604
DO - 10.1093/mnras/stw1604
M3 - Article
VL - 461
SP - 3864
EP - 3876
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 4
ER -