Stability of Standing Accretion Shocks, with an Eye toward Core-Collapse Supernovae

By J. Blondin, A. Mezzacappa, Christine DeMarino. 2002

581 citations recorded by the source corpus.

We examine the stability of standing, spherical accretion shocks. Accretion shocks arise in core-collapse supernovae (the focus of this paper), star formation, and accreting white dwarfs and neutron stars. We present a simple analytic model and use time-dependent hydrodynamics simulations to show that this solution is stable to radial perturbations. In two dimensions we show that small perturbations to a spherical shock front can lead to rapid growth of turbulence behind the shock, driven by the injection of vorticity from the now nonspherical shock. We discuss the ramifications this instability may have for the supernova mechanism.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9131e1e10016e36fccae36960233d0527ff44f30

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Citations in the corpus

DIMENSION AS A KEY TO THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2010, background): “…though we do see pre-explosion and blast asymmetries in 3D, we do not see a strong ` = 1 axially-symmetric “SASI” oscillation, such as is obtained in 2D in this paper and by others (Blondin et al. 2003; Bruenn et al. 2007,2010; Burrows et al. 2006,2007a; Buras et al. 2006ab; Marek & Janka 2009).”
Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A (2005, background): “…(Foglizzo & Tagger 2000; Foglizzo 2002; Foglizzo & Galetti 2003; Foglizzo et al. 2005; Ohnishi et al. 2005), and SASI instabilities (Blondin et al. 2003; Blondin & Mezzacappa 2005), can grow from small random perturbations behind the shock and result in a global anisotropy of the…”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “…Dessart et al. 2006), neutrino-driven convection in the postshock region between protoneutron star and shock (Herant et al. 1994; Burrows et al. 1995; Janka & Müller 1996), and the standing accretion shock instability (SASI, Blondin et al. 2003; Scheck et al. 2008) aid the neutrino mechanism.”
The Spherical Accretion Shock Instability in the Linear Regime (2005, background): “…in the post-bounce stellar core during the neutrino heating phase (as was shown in Paper I) but characterized by flat or positive entropy gradients, and as such convectively stable, Blondin et al. (2003) were able to isolate the dynamical behavior of the post-bounce accretion shock per se.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “A number of recent works (Cerdá-Durán et al. 2013; Kuroda et al. 2016, 2017; Pan et al. 2017; Andresen et al. 2017) pointed to a separate GW feature associated with the SASI (see more about the SASI phenomenon, for example, in Blondin et al. 2003; Foglizzo et al. 2007).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, methodology): “These works relied on asymmetries that developed only after core bounce by neutrino-driven convection and the standingaccretion shock instability (SASI; Blondin et al. 2003; Foglizzo 2002).”
Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, background): “More recently, Blondin et al. (2003) identified a new instability that may prove crucial for the viability of the neutrino mechanism.”
NEUTRINO-DRIVEN SUPERNOVA OF A LOW-MASS IRON-CORE PROGENITOR BOOSTED BY THREE-DIMENSIONAL TURBULENT CONVECTION (2015, background): “…to axial symmetry (2D) introduces nonradial flows and hydrodynamic instabilities like convection and the standing accretion shock instability (“SASI”; Blondin et al. 2003) in the neutrino-heated postshock layer, which have been recognized as helpful for the explosion due to improved…”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, methodology): “The morphology of our 180◦ model looks similar to the models published by Blondin et al. (2003), who studied the hydrodynamics of nonradial instabilities of accretion shocks without taking into account the effects of neutrino trans- port and neutrino heating.”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, methodology): “The process is very similar to the phenomenon identified as SASI in the idealized accretion setup studied by Blondin et al. (2003) and seen also in more sophisticated post-bounce accretion simulations by Scheck et al. (2008).”
THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR SUPERNOVA NEUTRINO TRANSPORT (2007, background): “…studied in three spatial dimensions, for example the pattern of the accretion flow (Herant et al. 1994), the standing accretion shock instability (Blondin et al. 2003), the excitation of PNS g-modes (Burrows et al. 2006), and the evolution of magnetic fields (see e.g. Kotake et al. (2006) and…”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “If the convection in the supernova engine develops low-mode instabilities, the resulting explosion can be asymmetric (Herant et al. 1992; Buras et al. 2003; Blondin et al. 2003).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…1996; Müller & Janka 1997), and that another more recently discovered large-scale instability, the standing accretion-shock instability (“SASI”, Blondin et al. 2003; Blondin & Mezzacappa 2006; Foglizzo et al. 2006; Ohnishi et al. 2006; Foglizzo et al. 2007; Scheck et al. 2008; Iwakami et…”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, methodology): “A new instability, the standing accretion shock instability (SASI), was discovered by Blondin et al. (2003), who carried out idealized 2D simulations of an accretion shock using an analytic EOS, neutrino cooling, but no neutrino heating.”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…convection (Burrows et al. 1995; Janka & Mueller 1996; Foglizzo et al. 2006; Radice et al. 2016, 2018), or the standing accretion shock instability (SASI; Blondin et al. 2003; Foglizzo et al. 2007; Burrows et al. 2012; Hanke et al. 2013; Abdikamalov et al. 2015) become fully developed.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…al. 2012; Murphy et al. 2013; Ott et al. 2013), the standing accretion shock instability (SASI) and/or vortical-acoustic instability (Foglizzo 2002; Blondin et al. 2003; Blondin & Mezzacappa 2006; Ohnishi et al. 2006; Iwakami et al. 2008; Marek & Janka 2009; Fernández 2010; Suwa et al. 2010;…”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS (2012, background): “…1990; Herant et al. 1992, 1994; Burrows et al. 1995; Janka & Müller 1996; Müller & Janka 1997), the standing accretion-shock instability (“SASI”, Blondin et al. 2003; Blondin & Mezzacappa 2006; Foglizzo et al. 2006; Ohnishi et al. 2006; Foglizzo et al. 2007; Scheck et al. 2008; Iwakami et…”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “…appears to hinge on the breaking of spherical symmetry by hydrodynamic instabilities like convection (Herant et al. 1994; Burrows et al. 1995; Janka & Müller 1996) and the standing accretion shock instability (SASI; Blondin et al. 2003; Foglizzo et al. 2007; Laming 2007; Guilet & Foglizzo 2012).”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, background): “…wave (Bethe 1990; Herant et al. 1992, 1994; Burrows et al. 1995; Janka & Müller 1995, 1996), and the standing accretion shock instability (SASI; Blondin et al. 2003; Foglizzo 2002; Blondin & Mezzacappa 2006; Ohnishi et al. 2006; Foglizzo et al. 2007; Scheck et al. 2008) causes an oscillatory…”