Linear analysis on the growth of non-spherical perturbations in supersonic accretion flows

Abstract

We analyzed the growth of non-spherical perturbations in supersonic accretion flows. We have in mind the application to the post-bounce phase of core-collapse supernovae (CCSNe). Such non-spherical perturbations have been suggested by a series of papers by Arnett, who has numerically investigated violent convections in the outer layers of pre-collapse stars. Moreover, Couch & Ott (2013) demonstrated in their numerical simulations that such perturbations may lead to a successful supernova even for a progenitor that fails to explode without the fluctuations. This study investigated the linear growth of perturbations during the infall onto a stalled shock wave. The linearized equations are solved as an initial and boundary value problem with the use of Laplace transform. The background is a Bondi accretion flow whose parameters are chosen to mimic the 15 ${\mathrm{M}}_{\odot }$ progenitor model by Woosley & Heger (2007), which is supposed to be a typical progenitor of CCSNe. We found that the perturbations that are given at a large radius grow as they flow down to the shock radius; the density perturbations can be amplified by a factor of 30, for example. We analytically showed that the growth rate is proportional to $l$, the index of the spherical harmonics. We also found that the perturbations oscillate in time with frequencies that are similar to those of the standing accretion shock instability. This may have an implication for shock revival in CCSNe, which will be investigated in our forthcoming paper in more detail.

arXiv comment11 pages, 9 figures, accepted for publication in The Astrophysical Journal

References in corpus (20)

• Stability of Standing Accretion Shocks, With an Eye Toward Core Collapse Supernovae
• Turbulent Convection in Stellar Interiors. I. Hydrodynamic Simulation
• Instability of a stalled accretion shock: evidence for the advective-acoustic cycle
• Towards Realistic Progenitors of Core-Collapse Supernovae
• Revival of The Stalled Core-Collapse Supernova Shock Triggered by Precollapse Asphericity in the Progenitor Star
• New Two-Dimensional Models of Supernova Explosions by the Neutrino-Heating Mechanism: Evidence for Different Instability Regimes in Collapsing Stellar Cores
• Active Carbon and Oxygen Shell Burning Hydrodynamics
• Two-Dimensional Hydrodynamics of Pre-Core Collapse: Oxygen Shell Burning
• Growth of Perturbation in Gravitational Collapse and Accretion
• Effect of Rotation on the Stability of a Stalled Cylindrical Shock and its Consequences for Core-Collapse Supernovae
• Effects of rotation on the revival of a stalled shock in supernova explosions
• On the linear growth mechanism driving the stationary accretion shock instability
• Further Adventures: Oxygen Burning in a Convective Shell
• A simple toy model of the advective-acoustic instability I. Perturbative approach
• Stability of the Accretion Flows with Stalled Shocks in Core-Collapse Supernovae
• Standing Accretion Shocks in the Supernova Core: Effects of Convection and Realistic EOS
• Post-shock-revival evolutions in the neutrino-heating mechanism of core-collapse supernovae
• A simple toy model of the advective-acoustic instability. II. Numerical simulations
• Parametric Study of Flow Patterns behind the Standing Accretion Shock Wave for Core-Collapse Supernovae
• Toward a magnetohydrodynamic theory of the stationary accretion shock: toy model of the advective-acoustic cycle in a magnetized flow

Cited by in corpus (20)

• The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations
• Supernova Simulations from a 3D Progenitor Model -- Impact of Perturbations and Evolution of Explosion Properties
• Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae
• The Status of Multi-Dimensional Core-Collapse Supernova Models
• Hydrodynamics of core-collapse supernovae and their progenitors
• The Last Minutes of Oxygen Shell Burning in a Massive Star
• One-, Two-, and Three-dimensional Simulations of Oxygen Shell Burning Just Before the Core-Collapse of Massive Stars
• Turbulence in Core-Collapse Supernovae
• Explosion mechanism of core-collapse supernovae: role of the Si/O interface
• Shock-Turbulence Interaction in Core-Collapse Supernovae
• 3D Simulations of Oxygen Shell Burning with and without Magnetic Fields
• 3D Simulations of Strongly Magnetised Non-Rotating Supernovae: Explosion Dynamics and Remnant Properties
• Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers
• The impact of vorticity waves on the shock dynamics in core-collapse supernovae
• Links between the shock instability in core-collapse supernovae and asymmetric accretions of envelopes
• Effects of rotation and magnetic field on the revival of a stalled shock in supernova explosions
• The impact of progenitor asymmetries on the neutrino-driven convection in core-collapse supernovae
• On the importance of progenitor asymmetry to shock revival in core-collapse supernovae
• Acoustic wave generation in collapsing massive stars with convective shells
• Impact of rotation on the evolution of convective vortices in collapsing stars