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

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 spira...

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Bibliographic Details
Published in:Astrophysics and space science 2009-08, Vol.322 (1-4), p.43-47
Main Authors: Iwakami, Wakana, Ohnishi, Naofumi, Kotake, Kei, Yamada, Shoichi, Sawada, Keisuke
Format: Article
Language:English
Subjects:
Accretion
Astrobiology
Astronomy
Astrophysics
Astrophysics and Astroparticles
Cosmology
Observations and Techniques
Original Article
Physics
Physics and Astronomy
Shock waves
Simulation
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Supernovae
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Summary: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.
ISSN:0004-640X
1572-946X
DOI:10.1007/s10509-008-9957-6