Spiral mode of standing accretion shock instability in core-collapse supernovae

Wakana Iwakami; Naofumi Ohnishi; Kei Kotake; Shoichi Yamada; Keisuke Sawada

doi:10.1007/s10509-008-9957-6

Spiral mode of standing accretion shock instability in core-collapse supernovae

Wakana Iwakami^*, Naofumi Ohnishi, Kei Kotake, Shoichi Yamada, Keisuke Sawada

^*Corresponding author for this work

School of Advanced Science and Engineering

Research output: Contribution to journal › Article › peer-review

9 Citations (Scopus)

Abstract

The study of standing accretion shock instability (SASI) in core-collapse supernova cores has been done with three-dimensional (3D) computer simulations. Rotations with various perturbations were introduced from outer boundary of an initial steady accreting flow. We found that one or two armed spiral accreting flow onto the proto-neutron star (PNS) is formed inside the shock wave depending on perturbations. The linear growth of spiral modes are clearly diagnosed by the mode analysis of the shock surface, and the lower m modes grow quickly in the linear regime.

Original language	English
Pages (from-to)	43-47
Number of pages	5
Journal	Astrophysics and Space Science
Volume	322
Issue number	1-4
DOIs	https://doi.org/10.1007/s10509-008-9957-6
Publication status	Published - 2009 Aug 1

Keywords

Hydrodynamics
Instability
Supernovae

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1007/s10509-008-9957-6

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abstract = "The study of standing accretion shock instability (SASI) in core-collapse supernova cores has been done with three-dimensional (3D) computer simulations. Rotations with various perturbations were introduced from outer boundary of an initial steady accreting flow. We found that one or two armed spiral accreting flow onto the proto-neutron star (PNS) is formed inside the shock wave depending on perturbations. The linear growth of spiral modes are clearly diagnosed by the mode analysis of the shock surface, and the lower m modes grow quickly in the linear regime.",

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author = "Wakana Iwakami and Naofumi Ohnishi and Kei Kotake and Shoichi Yamada and Keisuke Sawada",

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T1 - Spiral mode of standing accretion shock instability in core-collapse supernovae

AU - Iwakami, Wakana

AU - Ohnishi, Naofumi

AU - Kotake, Kei

AU - Yamada, Shoichi

AU - Sawada, Keisuke

PY - 2009/8/1

Y1 - 2009/8/1

N2 - The study of standing accretion shock instability (SASI) in core-collapse supernova cores has been done with three-dimensional (3D) computer simulations. Rotations with various perturbations were introduced from outer boundary of an initial steady accreting flow. We found that one or two armed spiral accreting flow onto the proto-neutron star (PNS) is formed inside the shock wave depending on perturbations. The linear growth of spiral modes are clearly diagnosed by the mode analysis of the shock surface, and the lower m modes grow quickly in the linear regime.

AB - The study of standing accretion shock instability (SASI) in core-collapse supernova cores has been done with three-dimensional (3D) computer simulations. Rotations with various perturbations were introduced from outer boundary of an initial steady accreting flow. We found that one or two armed spiral accreting flow onto the proto-neutron star (PNS) is formed inside the shock wave depending on perturbations. The linear growth of spiral modes are clearly diagnosed by the mode analysis of the shock surface, and the lower m modes grow quickly in the linear regime.

KW - Hydrodynamics

KW - Instability

KW - Supernovae

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SN - 0004-640X

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SP - 43

EP - 47

JO - Astrophysics and Space Science

JF - Astrophysics and Space Science

IS - 1-4

ER -

Spiral mode of standing accretion shock instability in core-collapse supernovae

Abstract

Keywords

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