Numerical Analysis of Standing Accretion Shock Instability with Neutrino Heating in Supernova Cores

By N. Ohnishi, K. Kotake, S. Yamada. 2005

142 citations recorded by the source corpus.

We have numerically studied the instability of the spherically symmetric standing accretion shock wave against nonspherical perturbations. We have in mind the application to collapse-driven supernovae in the postbounce phase, where the prompt shock wave generated by core bounce is commonly stalled. We take an experimental standpoint in this paper. Using spherically symmetric, completely steady, shocked accretion flows as unperturbed states, we have clearly observed both the linear growth and the subsequent nonlinear saturation of the instability. In so doing, we have employed a realistic equation of state, together with heating and cooling via neutrino reactions with nucleons. We have performed a mode analysis based on the spherical harmonics decomposition and found that the modes with l = 1,2 are dominant not only in the linear regime but also after nonlinear couplings generate various modes and saturation occurs. By varying the neutrino luminosity, we have constructed unperturbed states both with and without a negative entropy gradient. We have found that in both cases the growth of the instability is similar, suggesting that convection does not play a dominant role, which also appears to be supported by the recent linear analysis of the convection in accretion flows by Foglizzo et al. The oscillation period of the unstable l = 1 mode is found to fit better with the advection time rather than with the sound crossing time. Whatever the cause may be, the instability favors a shock revival.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ba032f6fa3ed0a9cc52c91b763a10d26a9954ac3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

IS STRONG SASI ACTIVITY THE KEY TO SUCCESSFUL NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS? (2011, background): “The predominant growth of such flows is typical of SASI activity, whose lowest-order spherical hrmonics modes possess the highest growth rates (Blondin et al. 2003; Blondin & Mezzacappa 2006b; Foglizzo et al. 2006, 2007; Ohnishi et al. 2006).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…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), or their combination…”
Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, methodology): “Ohnishi et al. (2006) executed time-dependent 1D simulations of the steady state solutions in Yamasaki & Yamada (2005) and observed similar pulsations, with amplitudes of order 10%.”
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).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…for this instability 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…”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, unknown): “…Fryer et al. (2002); Fryer (2004)) and the Standing-Accretion-ShockInstability (SASI, e.g., Blondin et al. (2003); Scheck et al. (2004, 2006); Ohnishi et al. (2006, 2007); Foglizzo et al. (2006); Iwakami et al. (2008, 2009); Murphy & Burrows (2008); Fernández & Thompson (2009b,a), and…”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “, [57, 58, 59, 60, 61, 62, 63, 64, 65, 66, 67, 68] see references t herein) can help the onset of the neutrino-driven explosion.”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, background): “…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 deformation with a dominance of…”
Instability of a Stalled Accretion Shock: Evidence for the Advective-Acoustic Cycle (2006, background): “The recent discovery of a strong l ¼ 1 instability of stalled accretion shocks in the context of core-collapse supernovae (Blondin et al. 2003; Scheck et al. 2004; Ohnishi et al. 2006; Burrows et al. 2006) has revived the interest in the fundamental stability properties of accretion shocks.”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “…in the neutrino-heating layer between the gain radius and the stalled supernova shock (Herant et al. 1994; Burrows et al. 1995; Janka & Müller 1996; Fryer & Warren 2002, 2004) as well as SASI activity (Blondin et al. 2003; Blondin & Mezzacappa 2006; Ohnishi et al. 2006; Scheck et al. 2008).”
Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the (2007, methodology): “…to consider a local quantity A(t,Rg(t), θ) in the postshock layer here rather than the shock displacement δR = Rs(θ)−〈Rs〉θ (used in Blondin et al. 2003 and Ohnishi et al. 2006), because A is much less affected by noise (A(t) = 0 for a non-stationary spherical flow, whereas Rs(t) is varying) and…”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, background): “…description of the neutrino physics and of the equation of state of the supernova medium, Scheck et al. (2004); Janka et al. (2005b, 2004b, 2005a), Ohnishi et al. (2006), Buras et al. (2006b), and Burrows et al. (2006) provide results that demonstrate that the instability of the accretion shock…”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, background): “The development of large-scale anisotropies withl = 1, 2 modes was also seen in other 2D simulations (Blondin et al. 2003; Scheck et al. 2004; Ohnishi et al. 2006; Burrows et al. 2006) and occurred in some preliminary 3D simulations (Mezzacappa & Blondin 2003, L. Scheck, private communication), too.”
A Survey About Nothing: Monitoring a Million Supergiants for Failed Supernovae (2008, background): “…2000; Liebendörfer et al. 2001; Thompson et al. 2003; Sumiyoshi et al. 2005; in 2D: e.g., Fryer 1999; Buras et al. 2003, 2006; Livne et al. 2004; Ohnishi et al. 2006; and in 3D: e.g., Fryer & Warren 2002) it is dif- 4 There is the intriguing observation by Muno et al. (2006) of a probable…”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “…to larger average shock radii, increase the dwell time of material in the gain region, may lead to secondary shocks, and are thus generally aiding the explosion mechanism (Ohnishi et al. 2006; Scheck et al. 2006; Murphy & Burrows 2008; Ott et al. 2008; Marek & Janka 2009; B. Müller et al. 2012b).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, unknown): “…references in Burrows et al. (2012); Murphy et al. (2013); Couch (2013)) and the SASI (e.g., Blondin et al. (2003); Scheck et al. (2004, 2006); Ohnishi et al. (2006, 2007); Ott et al. (2008); Murphy & Burrows (2008); Foglizzo et al. (2006, 2007, 2012); Iwakami et al. (2008, 2009, 2013);…”