Two-dimensional versus three-dimensional supernova hydrodynamic instability growth

J. Kane, W David Arnett, B. A. Remington, S. G. Glendinning, G. Bazán, E. Müller, B. A. Fryxell, R. Teyssier

Research output: Contribution to journalArticle

64 Citations (Scopus)

Abstract

Numerical simulations using the SN hydrodynamics code PROMETHEUS are carried out to study the difference between growth of two-dimensional versus three-dimensional single-mode perturbations at the He-H and O-He interfaces of SN 1987A. We find that in the rest frame of an unperturbed one-dimensional interface, a three-dimensional single-mode perturbation grows ≈30%-35% faster than a two-dimensional single-mode perturbation, when the wavelengths are chosen to give the same linear stage growth in the planar limit. In simulations where we impose single-mode density perturbations in the O layer of the initial model and random velocity perturbations in the postshock fluid near the He-H interface, we find that both axisymmetric O spikes and three-dimensional O spikes penetrate significantly further than two-dimensional O spikes. The difference between two dimensions and three dimensions predicted by our calculations is not enough to account for the difference between observed 56Co velocities in SN 1987A and the results of previous two-dimensional simulations of SN 1987A, but our results suggest that the real three-dimensional hydrodynamics are noticeably different than the two-dimensional simulations predict.

Original languageEnglish (US)
Pages (from-to)989-994
Number of pages6
JournalAstrophysical Journal
Volume528
Issue number2 PART 1
StatePublished - Jan 10 2000

Fingerprint

supernovae
hydrodynamics
perturbation
spikes
simulation
wavelength
fluid
fluids
wavelengths

Keywords

  • Hydrodynamics
  • Instabilities
  • Methods: Numerical
  • Supernovae: General

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Kane, J., Arnett, W. D., Remington, B. A., Glendinning, S. G., Bazán, G., Müller, E., ... Teyssier, R. (2000). Two-dimensional versus three-dimensional supernova hydrodynamic instability growth. Astrophysical Journal, 528(2 PART 1), 989-994.

Two-dimensional versus three-dimensional supernova hydrodynamic instability growth. / Kane, J.; Arnett, W David; Remington, B. A.; Glendinning, S. G.; Bazán, G.; Müller, E.; Fryxell, B. A.; Teyssier, R.

In: Astrophysical Journal, Vol. 528, No. 2 PART 1, 10.01.2000, p. 989-994.

Research output: Contribution to journalArticle

Kane, J, Arnett, WD, Remington, BA, Glendinning, SG, Bazán, G, Müller, E, Fryxell, BA & Teyssier, R 2000, 'Two-dimensional versus three-dimensional supernova hydrodynamic instability growth', Astrophysical Journal, vol. 528, no. 2 PART 1, pp. 989-994.
Kane J, Arnett WD, Remington BA, Glendinning SG, Bazán G, Müller E et al. Two-dimensional versus three-dimensional supernova hydrodynamic instability growth. Astrophysical Journal. 2000 Jan 10;528(2 PART 1):989-994.
Kane, J. ; Arnett, W David ; Remington, B. A. ; Glendinning, S. G. ; Bazán, G. ; Müller, E. ; Fryxell, B. A. ; Teyssier, R. / Two-dimensional versus three-dimensional supernova hydrodynamic instability growth. In: Astrophysical Journal. 2000 ; Vol. 528, No. 2 PART 1. pp. 989-994.
@article{2c7f56c6a06045f2ae5849a7e7884f39,
title = "Two-dimensional versus three-dimensional supernova hydrodynamic instability growth",
abstract = "Numerical simulations using the SN hydrodynamics code PROMETHEUS are carried out to study the difference between growth of two-dimensional versus three-dimensional single-mode perturbations at the He-H and O-He interfaces of SN 1987A. We find that in the rest frame of an unperturbed one-dimensional interface, a three-dimensional single-mode perturbation grows ≈30{\%}-35{\%} faster than a two-dimensional single-mode perturbation, when the wavelengths are chosen to give the same linear stage growth in the planar limit. In simulations where we impose single-mode density perturbations in the O layer of the initial model and random velocity perturbations in the postshock fluid near the He-H interface, we find that both axisymmetric O spikes and three-dimensional O spikes penetrate significantly further than two-dimensional O spikes. The difference between two dimensions and three dimensions predicted by our calculations is not enough to account for the difference between observed 56Co velocities in SN 1987A and the results of previous two-dimensional simulations of SN 1987A, but our results suggest that the real three-dimensional hydrodynamics are noticeably different than the two-dimensional simulations predict.",
keywords = "Hydrodynamics, Instabilities, Methods: Numerical, Supernovae: General",
author = "J. Kane and Arnett, {W David} and Remington, {B. A.} and Glendinning, {S. G.} and G. Baz{\'a}n and E. M{\"u}ller and Fryxell, {B. A.} and R. Teyssier",
year = "2000",
month = "1",
day = "10",
language = "English (US)",
volume = "528",
pages = "989--994",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2 PART 1",

}

TY - JOUR

T1 - Two-dimensional versus three-dimensional supernova hydrodynamic instability growth

AU - Kane, J.

AU - Arnett, W David

AU - Remington, B. A.

AU - Glendinning, S. G.

AU - Bazán, G.

AU - Müller, E.

AU - Fryxell, B. A.

AU - Teyssier, R.

PY - 2000/1/10

Y1 - 2000/1/10

N2 - Numerical simulations using the SN hydrodynamics code PROMETHEUS are carried out to study the difference between growth of two-dimensional versus three-dimensional single-mode perturbations at the He-H and O-He interfaces of SN 1987A. We find that in the rest frame of an unperturbed one-dimensional interface, a three-dimensional single-mode perturbation grows ≈30%-35% faster than a two-dimensional single-mode perturbation, when the wavelengths are chosen to give the same linear stage growth in the planar limit. In simulations where we impose single-mode density perturbations in the O layer of the initial model and random velocity perturbations in the postshock fluid near the He-H interface, we find that both axisymmetric O spikes and three-dimensional O spikes penetrate significantly further than two-dimensional O spikes. The difference between two dimensions and three dimensions predicted by our calculations is not enough to account for the difference between observed 56Co velocities in SN 1987A and the results of previous two-dimensional simulations of SN 1987A, but our results suggest that the real three-dimensional hydrodynamics are noticeably different than the two-dimensional simulations predict.

AB - Numerical simulations using the SN hydrodynamics code PROMETHEUS are carried out to study the difference between growth of two-dimensional versus three-dimensional single-mode perturbations at the He-H and O-He interfaces of SN 1987A. We find that in the rest frame of an unperturbed one-dimensional interface, a three-dimensional single-mode perturbation grows ≈30%-35% faster than a two-dimensional single-mode perturbation, when the wavelengths are chosen to give the same linear stage growth in the planar limit. In simulations where we impose single-mode density perturbations in the O layer of the initial model and random velocity perturbations in the postshock fluid near the He-H interface, we find that both axisymmetric O spikes and three-dimensional O spikes penetrate significantly further than two-dimensional O spikes. The difference between two dimensions and three dimensions predicted by our calculations is not enough to account for the difference between observed 56Co velocities in SN 1987A and the results of previous two-dimensional simulations of SN 1987A, but our results suggest that the real three-dimensional hydrodynamics are noticeably different than the two-dimensional simulations predict.

KW - Hydrodynamics

KW - Instabilities

KW - Methods: Numerical

KW - Supernovae: General

UR - http://www.scopus.com/inward/record.url?scp=0034627504&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0034627504&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0034627504

VL - 528

SP - 989

EP - 994

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART 1

ER -