The Spherical Accretion Shock Instability in the Linear Regime

By J. Blondin, A. Mezzacappa. 2005

147 citations recorded by the source corpus.

We use time-dependent, axisymmetric, hydrodynamic simulations to study the linear stability of the stalled, spherical accretion shock that arises in the postbounce phase of core-collapse supernovae. We show that this accretion shock is stable to radial modes, with decay rates and oscillation frequencies in close agreement with the linear stability analysis of Houck and Chevalier. For nonspherical perturbations we find that the l = 1 mode is always unstable for parameters appropriate to core-collapse supernovae. We also find that the l = 2 mode is unstable, but typically has a growth rate smaller than that for l = 1. Furthermore, the l = 1 mode is the only mode found to transition into a nonlinear stage in our simulations. This result provides a possible explanation for the dominance of an l = 1 "sloshing" mode seen in many two-dimensional simulations of core-collapse supernovae.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4439e7f64a0cb97e4f6d696acf69969cff48f5a1

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Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, background): “…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 growth of nonradial shock…”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “SASI was found to possess the highest growth rates for the lowest-order (dipole and quadrupole) spherical harmonics (Blondin & Mezzacappa 2006; Foglizzo et al. 2007; Iwakami et al. 2008) and to give rise to spiral-mode mass motions in 3D simulations (Blondin & Mezzacappa 2007; Iwakami et al. 2009;…”
Ultra-stripped supernovae: progenitors and fate (2015, background): “…non-radial hydrodynamic instabilities in the collapsing stellar core (i.e.n utrinodriven convection and the standing accretion-shock instability, Blondin & Mezzacappa 2006; Scheck et al. 2006; Foglizzo et al. 2007; Marek & Janka 2009; Janka 2012, 2013; Bruenn et al. 2014; Foglizzo et al. 2015).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…& 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 al. 2008, 2009;…”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “…the fastest growth for the higher- modes (see Foglizzo et al. 2006), the SASI is expected to possess the largest growth rates for the dipolar and quadrupolar deformations (corresponding to = 1, 2; Blondin & Mezzacappa 2006; Foglizzo et al. 2007; Yamasaki & Foglizzo 2008; Foglizzo 2001, 2002).”
IS STRONG SASI ACTIVITY THE KEY TO SUCCESSFUL NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS? (2011, background): “…of the shock can cause strong shockheating of the postshock matter as discussed in detail by Scheck et al. (2008), Blondin et al. (2003), and Blondin & Mezzacappa (2006b), thus not only massively affecting the postshock flow but also providing an additional entropy source besides…”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…Foglizzo et al. 2007; Iwakami et al. 2008b; Scheck et al. 2008; Yamasaki & Foglizzo 2008; Foglizzo 2009; Sato et al. 2009) or purely acoustic cycle (Blondin & Mezzacappa 2006; Laming 2007), though recent linear and nonlinear analysis of simple models suggest that the advective-acoustic cycle is…”
Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, background): “It is the standing accretion shock instability (SASI), which may be an advective-acoustic (Foglizzo & Tagger 2000; Foglizzo 2002; Foglizzo et al. 2007) or purely acoustic cycle (Blondin & Mezzacappa 2006).”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, background): “The authors referred to this as the “standing accretion shock instability”, or SASI, which reveals a preferred growth of l = 1 mode deformation and which was explained by Blondin & Mezzacappa (2006) as a consequence of the propagation of sound waves in the volume enclosed by the shock.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…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; Hanke et al. 2012, 2013),…”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, methodology): “…the absence of neutrino heating, a result that has been confirmed by further hydrodynamical simulations in a number of follow-up studies in 2D and 3D (Blondin & Mezzacappa 2006; Ohnishi et al. 2006; Blondin & Mezzacappa 2007; Scheck et al. 2008; Iwakami et al. 2008, 2009; Fernández & Thompson…”
Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the (2007, methodology): “Can the instability be identified as consequence of an amplifying advective-acoustic cycle, of a growing standing pressure wave (Blondin & Mezzacappa 2006) or of something else?”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, methodology): “In contrast, Blondin & Mezzacappa (2006) and Blondin & Shaw (2007) advocate a purely acoustic cycle as the cause of the low-mode SASI and see this hypothesis supported by their numerical studies.”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “…road towards short neutron star birth periods of a few tens of milliseconds other than spin-up by the standing accretion shock instability (Blondin & Mezzacappa 2006; Guilet & Fernández 2014; Kazeroni et al. 2016) or the assumption of pre-collapse rotation rates of ∼100 s (Heger et al.…”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, background): “…characteristic oscillatory growth of this instability is thought to be mediated by an amplifying advective-acoustic cycle (Foglizzo 2002; Foglizzo et al. 2006, 2007; Guilet & Foglizzo 2012; see, however, Blondin & Mezzacappa 2006 and Laming 2007 for the interpretation as a purely acoustic cycle).”