The Standing Accretion Shock Instability: Enhanced Growth in Rotating Progenitors

被引：14

作者：

Blondin, John M. ^{[1
]}

Gipson, Emily ^{[1
]}

Harris, Sawyer ^{[1
]}

Mezzacappa, Anthony ^{[2
,3
]}

机构：

[1] North Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA

[2] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA

[3] Oak Ridge Natl Lab, Joint Inst Computat Sci, POB 2008, Oak Ridge, TN 37831 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 835卷 / 02期

基金：

美国国家科学基金会;

关键词：

accretion; accretion disks; hydrodynamics; shock waves; supernovae: general Supporting material: interactive figures; CORE-COLLAPSE SUPERNOVAE; ACOUSTIC CYCLE; STABILITY; MODES;

D O I：

10.3847/1538-4357/835/2/170

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate the effect of progenitor rotation on the standing accretion shock instability (SASI) using two-and three-dimensional hydrodynamic simulations. We find that the growth rate of the SASI is a near-linearly increasing function of the specific angular momentum in the accreting gas. Both the growth rate and the angular frequency in the two-dimensional model with cylindrical geometry agree well with previous linear stability analyses. When excited by very small random perturbations, a one-armed spiral mode dominates the small rotation rates predicted by current stellar evolution models, while progressively higher-order modes are seen as the specific angular momentum increases.

引用

页数：5

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