Instability of a Stalled Accretion Shock: Evidence for the Advective-Acoustic Cycle

By T. Foglizzo, P. Galletti, L. Scheck, Hans-Thomas Janka. 2006

215 citations recorded by the source corpus.

We analyze the linear stability of a stalled accretion shock in a perfect gas with a parameterized cooling function ℒ ∝ ρβ-αPα. The instability is dominated by the l = 1 mode if the shock radius exceeds 2-3 times the accretor radius, depending on the parameters of the cooling function. The growth rate and oscillation period are comparable to those observed in the numerical simulations of Blondin & Mezzacappa. The instability mechanism is analyzed by separately measuring the efficiencies of the purely acoustic cycle and the advective-acoustic cycle. These efficiencies are estimated directly from the eigenspectrum and also through a WKB analysis in the high-frequency limit. Both methods prove that the advective-acoustic cycle is unstable and that the purely acoustic cycle is stable. Extrapolating these results to low frequency leads us to interpret the dominant mode as an advective-acoustic instability, different from the purely acoustic interpretation of Blondin & Mezzacappa. A simplified characterization of the instability is proposed, based on an advective-acoustic cycle between the shock and the radius r∇ where the velocity gradients of the stationary flow are strongest. The importance of the coupling region in this mechanism calls for a better understanding of the conditions for an efficient advective-acoustic coupling in a decelerated, nonadiabatic flow, in order to extend these results to core-collapse supernovae.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7f995c1ba513fc2b7c4f2b45e4b6f89788908b46

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Citations in the corpus

Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “…1995; Janka & Müller 1996; Buras et al. 2006a) and the recently identified standing accretion shockinstability (SASI, e.g., Foglizzo & Tagger 2000; Foglizzo et al. 2007; Scheck et al. 2008; Blondin et al. 2003; Burrows et al. 2007c; Iwakami et al. 2008) lead to a dwell time of accreting outer…”
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).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “The neutrino-heating region is unstable to convection, and the presence of convective motions produces vorticity and entropy perturbations that feed back into the advective-acoustic cycle that is considered as an explanation of the SASI phenomenon (see Foglizzo 2001, 2002; Foglizzo et al. 2007).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “This can lead to a suppression of the growth of the SASI (cf., Foglizzo et al. 2007; Fernández et al. 2014).”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, background): “0 (Foglizzo et al. 2007; Scheck et al. 2008; Guilet & Foglizzo 2012).”
Colloquium: Perspectives on core-collapse supernova theory (2012, background): “…instability (“SASI”), that has been welldiagnosed and studied by Foglizzo (2002,2009), Blondin & Mezzacappa (2006), Foglizzo, Scheck, & Janka (2006), Foglizzo et al. (2007), Yamasaki & Foglizzo (2008), Scheck et al. (2008), Iwakami et al. (2008), Kotake et al. (2009), and Foglizzo et al. (2012).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…is debated to be either an advective-acoustic cycle (Foglizzo & Tagger 2000; Foglizzo 2001, 2002; Blondin et al. 2003; Ohnishi et al. 2006; 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…”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “…amplify perturbations in the shock front, thus creating a feedback cycle that injects power preferentially into loworder modes (see Foglizzo 2002; Foglizzo et al. 2006, 2007; Ohnishi et al. 2006; Yamasaki & Yamada 2007; Fernández & Thompson 2009b,a; Scheck et al. 2008; Guilet & Foglizzo 2012 and…”
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).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “Similarly, the SASI is an acousticadvective cycle (e.g. Foglizzo 2002; Foglizzo et al. 2006, 2007) and as such depends on the rate with which matter is advected.”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS (2012, background): “…& 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 al. 2008, 2009; Fernández & Thompson 2009; Fernández 2010).”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “The non-radial flow instabilities (convective overturn and the standing accretion shock instability, SASI; Blondin et al. 2003; Foglizzo 2002; Foglizzo et al. 2006, 2007; Scheck et al. 2008) that develop shortly after core bounce in the postshock accretion layer of collapsing stellar cores,…”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, background): “Although the theoretical understanding of the growth conditions of the SASI and neutrino-driven convection is mostly based on linear theory (e.g., Foglizzo et al. 2007; Laming 2007; Yamasaki & Yamada 2007; Yamasaki & Foglizzo 2008; Guilet & Foglizzo 2012), the predictions were found to be…”
Formation of Double Neutron Star Systems (2017, background): “…non-radial hydrodynamic instabilities in the collapsing stellar core (i.e. neutrino-driven 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).”
Science case for the Einstein telescope (2019, background): “Besides, the Standing Accretion Shock Instability (SASI) [127, 128] which is an instability of the supernova shock wave itself is expected, in conjunction with turbulence, to modulate the accretion flow, to excite the proto-neutro star high frequency oscillation modes as well as to generate low freq”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, unknown): “Foglizzo et al. (2007) explain the SASI by an advective-acoustic cycle (see also Foglizzo 2001, 2002, 2008).”