2013/08/31 by Wakana Iwakami, Hiroki Nagakura, Shoichi Yamada · 24 citations
Physics and Astronomy · #Accretion (finance) #Astrophysics #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Convection #Flow (mathematics) #Gamma-ray bursts and supernovae #Instability #Mechanics #Neutrino #Physics #Shock (circulatory) #Shock wave #Supernova #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/786/2/118
published in The Astrophysical Journal 786(2), 118 (IOP Publishing) · Accepted for publication in ApJ, 54 pages, 20 figures, 3 table
arxiv created 2014/03/19 · openalex publication_date 2014/04/24 · arxiv updated 2014/09/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
In this study, we conduct three-dimensional hydrodynamic simulations systematically to investigate the flow patterns behind the accretion shock waves that are commonly formed in the post-bounce phase of core-collapse supernovae. Adding small perturbations to spherically symmetric, steady, shocked accretion flows, we compute the subsequent evolutions to find what flow pattern emerges as a consequence of hydrodynamical instabilities such as convection and standing accretion shock instability for different neutrino luminosities and mass accretion rates. Depending on these two controlling parameters, various flow patterns are indeed realized. We classify them into three basic patterns and two intermediate ones; the former includes sloshing motion (SL), spiral motion (SP), and multiple buoyant bubble formation (BB); the latter consists of spiral motion with buoyant-bubble formation (SPB) and spiral motion with pulsationally changing rotational velocities (SPP). Although the post-shock flow is highly chaotic, there is a clear trend in the pattern realization. The sloshing and spiral motions tend to be dominant for high accretion rates and low neutrino luminosities, and multiple buoyant bubbles prevail for low accretion rates and high neutrino luminosities. It is interesting that the dominant pattern is not always identical between the semi-nonlinear and nonlinear phases near the critical luminosity; the intermediate cases are realized in the latter case. Running several simulations with different random perturbations, we confirm that the realization of flow pattern is robust in most cases.