Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the

By L. Scheck, Hans-Thomas Janka, T. Foglizzo, K. K. M. F. Astrophysics, Garching Service d'Astrophysique, CEA-Saclay. 2007

168 citations recorded by the source corpus.

Performing two-dimensional hydrodynamic simulations including a detailed treatment of the equation of state of the stellar plasma and for the neutrino transport and interactions, we investigate here the interplay between different kinds of non-radial hydrodynamic instabilities that can play a role during the postbounce accretion phase of collapsing stellar cores. The convective mode of instability, which is driven by the negative entropy gradients caused by neutrino heating or by variations in the shock strength in transient phases of shock expansion and contraction, can be identified clearly by the development of typical Rayleigh-Taylor mushrooms. However, in those cases where the gas in the postshock region is rapidly advected towards the gain radius, the growth of such a buoyancy instability can be suppressed. In this situation the shock and postshock flow can nevertheless develop non-radial asymmetry with an oscillatory growth in the amplitude. This phenomenon has been termed “standing (or spherical) accretion shock instability” (SASI). It is shown here that the SASI oscillations can trigger convective instability, and like the latter, they lead to an increase in the average shock radius and in the mass of the gain layer. Both hydrodynamic instabilities in combination stretch the advection time of matter accreted through the neutrino-heating layer and thus enhance the neutrino energy deposition in support of the neutrino-driven explosion mechanism. A rapidly contracting and more compact nascent neutron star turns out to be favorable for explosions, because the accretion luminosity and neutrino heating are greater and the growth rate of the SASI is higher. Moreover, we show that the oscillation period of the SASI observed in our simulations agrees with the one estimated for the advective-acoustic cycle (AAC), in which perturbations are carried by the accretion flow from the shock to the neutron star and pressure waves close an amplifying global feedback loop. A variety of other features in our models, as well as differences in their behavior, can also be understood on the basis of the AAC hypothesis. The interpretation of the SASI in our simulations as a purely acoustic phenomenon, however, appears difficult.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/014f37a33a2193d00dd0b9eadd2a89086e5cee14

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Citations in the corpus

Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, methodology): “Scheck et al. (2008) compared these quantities for 1D and 2D simulations with the same neutrino luminosity and found similar bifurcations in these integral measures.”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “…and, again, can enhance the efficiency of neutrino-energy deposition (Marek & Janka 2009) even when convection is weak or its growth is suppressed because of a small shock-stagnation radius and correspondingly fast infall velocities in the gain layer (Foglizzo et al. 2006; Scheck et al. 2008).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “At the beginning of the runs, the SASI-driven deviation from sphericity of the stalled shock is mild, but grows with time, showing ℓ = 1 excursions now generally recognized as characteristic of the SASI10 (Scheck et al. 2008; Marek & Janka 2007; Bruenn et al. 2006; Burrows et al. 2007c).”
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).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “• The growth of the SASI is favored by fast advection flows, because its growth rate in an advectiveacoustic cycle scales roughly inversely with the advection timescale of the accretion flow from the shock to the neutron star surface (e.g., Scheck et al. 2008).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “2), thus improving the simpler, time-dependent boundary neutrino luminosity prescribed by Kifonidis et al. (2006), Scheck et al. (2004, 2006, 2008), and Arcones et al. (2007); Arcones & Janka (2011) and the even simpler neutrino light-bulb treatment (without any transport approximation) applied by…”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “Foglizzo et al. (2006) argued that the strength of postshock convection is increased by large preshock perturbations and this dependence was first demonstrated by Scheck et al. (2008).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…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 (Blondin & Mezzacappa 2006; Laming 2007),…”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, background): “…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 low-order spherical harmonic modes.”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “These act as seeds for secondary convection (Scheck et al. 2008) and have been found to aid the neutrino-heating mechanism for powering supernova explosions (Scheck et al. 2008; Marek & Janka 2007; see also Murphy & Burrows 2008).”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “…modes excited by the infalling perturbations are already unstable to begin with and could be triggered by weaker infalling perturbations, whereas advection stabilises these modes in the SASI-dominated regime (Foglizzo et al. 2006) unless the flow is strongly perturbed (Scheck et al. 2008).”
REVIVAL OF THE STALLED CORE-COLLAPSE SUPERNOVA SHOCK TRIGGERED BY PRECOLLAPSE ASPHERICITY IN THE PROGENITOR STAR (2013, background): “As pointed out by Foglizzo et al. (2006) and first demonstrated by Scheck et al. (2008), the development and strength of neutrino-driven convection in the gain layer increases with increasing magnitude of the accreting seed perturbations.”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, methodology): “…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 2009b; Fernández 2010).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…(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 (Scheck et al. 2008; Müller et al. 2012b; Iwakami et al. 2014; Fernández et al. 2014).”
A Survey About Nothing: Monitoring a Million Supergiants for Failed Supernovae (2008, background): “…although recently a 2D calculation of a relatively lowmass progenitor (11.2M⊙) led to a weak neutrino-driven explosion (Buras et al. 2006) and there may be new mechanisms associated with less restrictive simulation geometries (Blondin et al. 2003; Burrows et al. 2006; Scheck et al. 2008).”