SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES

The relevance of the standing accretion shock instability (SASI) compared to neutrino-driven convection in three-dimensional (3D) supernova-core environments is still highly controversial. Studying a 27 M ☉ progenitor, we demonstrate, for the first time, that violent SASI activity can develop in 3D simulations with detailed neutrino transport despite the presence of convection. This result was obtained with the PROMETHEUS-VERTEX code with the same sophisticated neutrino treatment so far used only in one-dimensional and two-dimensional (2D) models. While buoyant plumes initially determine the nonradial mass motions in the postshock layer, bipolar shock sloshing with growing amplitude sets in during a phase of shock retraction and turns into a violent spiral mode whose growth is only quenched when the infall of the Si/SiO interface leads to strong shock expansion in response to a dramatic decrease of the mass accretion rate. In the phase of large-amplitude SASI sloshing and spiral motions, the postshock layer exhibits nonradial deformation dominated by the lowest-order spherical harmonics (l = 1, m = 0, ±1) in distinct contrast to the higher multipole structures associated with neutrino-driven convection. We find that the SASI amplitudes, shock asymmetry, and nonradial kinetic energy in three dimensions can exceed those of the corresponding 2D case during extended periods of the evolution. We also perform parameterized 3D simulations of a 25 M ☉ progenitor, using a simplified, gray neutrino transport scheme, an axis-free Yin-Yang grid, and different amplitudes of random seed perturbations. They confirm the importance of the SASI for another progenitor, its independence of the choice of spherical grid, and its preferred growth for fast accretion flows connected to small shock radii and compact proto-neutron stars as previously found in 2D setups.

[1]  L. Scheck,et al.  Neutrino-driven Convection versus Advection in Core-Collapse Supernovae , 2005, astro-ph/0507636.

[2]  E. Müller,et al.  Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions , 2006, astro-ph/0601302.

[3]  K. Kotake,et al.  FULLY GENERAL RELATIVISTIC SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE WITH AN APPROXIMATE NEUTRINO TRANSPORT , 2012, 1202.2487.

[4]  Non-radial instabilities of isothermal Bondi accretion with a shock: Vortical-acoustic cycle vs. post-shock acceleration , 2002, astro-ph/0206274.

[5]  H. Janka,et al.  Radiation hydrodynamics with neutrinos - Variable Eddington factor method for core-collapse supernova simulations , 2002, astro-ph/0203101.

[6]  M. Rampp,et al.  Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star , 2005, astro-ph/0507135.

[7]  Department of Astrophysical Sciences,et al.  Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores , 2008, 0804.0239.

[8]  October I.  Physical Review Letters , 2022 .

[9]  E. Müller,et al.  Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products , 2012, 1210.8148.

[10]  A. Marek,et al.  DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY , 2007, 0708.3372.

[11]  A. Burrows,et al.  On the nature of core-collapse supernova explosions , 1995, astro-ph/9506061.

[12]  CEA-Saclay,et al.  Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the , 2007, 0704.3001.

[13]  H. Janka,et al.  PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS , 2012, 1205.3657.

[14]  A. Burrows,et al.  Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism , 2008, 0805.3345.

[15]  Explosions of O-Ne-Mg cores, the Crab supernova, and subluminous type II-P supernovae , 2005, astro-ph/0512065.

[16]  Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A , 2005, astro-ph/0511369.

[17]  K. Kotake,et al.  Explosion Geometry of a Rotating 13 $\ M_{\odot}$ Star Driven by the SASI-Aided Neutrino-Heating Supernova Mechanism , 2009, 0912.1157.

[18]  A. Burrows,et al.  AN INVESTIGATION INTO THE CHARACTER OF PRE-EXPLOSION CORE-COLLAPSE SUPERNOVA SHOCK MOTION , 2012, 1204.3088.

[19]  L. Scheck,et al.  Instability of a Stalled Accretion Shock: Evidence for the Advective-Acoustic Cycle , 2006, astro-ph/0606640.

[20]  W. Benz,et al.  Inside the Supernova: A Powerful Convective Engine , 1994, astro-ph/9404024.

[21]  R. Fern'andez,et al.  STABILITY OF A SPHERICAL ACCRETION SHOCK WITH NUCLEAR DISSOCIATION , 2008, 0811.2795.

[22]  W. Benz,et al.  Postcollapse hydrodynamics of SN 1987A : two-dimensional simulations of the early evolution , 1992 .

[23]  Timothy D. Brandt,et al.  The hydrodynamic origin of neutron star kicks , 2011, 1112.3342.

[24]  Exploring the relativistic regime with Newtonian hydrodynamics: an improved effective gravitational potential for supernova simulations , 2005, astro-ph/0502161.

[25]  A. Burrows,et al.  An Instability in Neutron Stars at Birth , 1992, Science.

[26]  T. Foglizzo,et al.  On the linear growth mechanism driving the standing accretion shock instability , 2011, 1112.1427.

[27]  S. Yamada,et al.  Stability of Accretion Flows with Stalled Shocks in Core-Collapse Supernovae , 2006, astro-ph/0606581.

[28]  Timothy D. Brandt,et al.  RESULTS FROM CORE-COLLAPSE SIMULATIONS WITH MULTI-DIMENSIONAL, MULTI-ANGLE NEUTRINO TRANSPORT , 2010, 1009.4654.

[29]  A. Burrows,et al.  THE DOMINANCE OF NEUTRINO-DRIVEN CONVECTION IN CORE-COLLAPSE SUPERNOVAE , 2012, 1205.3491.

[30]  Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric , 2006, astro-ph/0612582.

[31]  Sean M. Couch,et al.  ON THE IMPACT OF THREE DIMENSIONS IN SIMULATIONS OF NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS , 2012, 1212.0010.

[32]  K. Kotake,et al.  THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT , 2011, 1108.3989.

[33]  Caltech,et al.  GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE , 2012, 1210.6674.

[34]  J. Laming.  Analytic Approach to the Stability of Standing Accretion Shocks: Application to Core-Collapse Supernovae , 2007, astro-ph/0701264.

[35]  K. Kotake,et al.  Three-Dimensional Simulations of Standing Accretion Shock Instability in Core-Collapse Supernovae , 2007, 0710.2191.

[36]  H. Janka,et al.  A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS , 2012, 1210.6984.

[37]  T. Foglizzo,et al.  Effect of Rotation on the Stability of a Stalled Cylindrical Shock and Its Consequences for Core-Collapse Supernovae , 2007, 0710.3041.

[38]  H. Janka,et al.  Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae , 2008, 0808.4136.

[39]  R. Fern'andez.  THE SPIRAL MODES OF THE STANDING ACCRETION SHOCK INSTABILITY , 2010, 1003.1730.

[40]  H. Janka,et al.  Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows - II. The reverse shock in two-dimensional simulations , 2010, 1008.0882.

[41]  C. Ott,et al.  A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE , 2009, 0907.4762.

[42]  A. Mezzacappa,et al.  Pulsar spins from an instability in the accretion shock of supernovae , 2006, Nature.

[43]  B. Fryxell,et al.  Instabilities and nonradial motion in SN 1987A , 1989 .

[44]  A. Burrows,et al.  DIMENSIONAL DEPENDENCE OF THE HYDRODYNAMICS OF CORE-COLLAPSE SUPERNOVAE , 2012, 1210.5241.

[45]  H. Janka,et al.  Parametrized 3D models of neutrino-driven supernova explosions - Neutrino emission asymmetries and gravitational-wave signals , 2011, 1106.6301.

[46]  R. Fern'andez,et al.  DYNAMICS OF A SPHERICAL ACCRETION SHOCK WITH NEUTRINO HEATING AND ALPHA-PARTICLE RECOMBINATION , 2008, 0812.4574.

[47]  M. Rampp,et al.  Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars , 2006 .

[48]  A. Burrows,et al.  DIMENSION AS A KEY TO THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVA EXPLOSIONS , 2010, 1006.3792.

[49]  H. Janka,et al.  NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES , 2012, 1205.7078.

[50]  Chris L. Fryer,et al.  Core-Collapse Simulations of Rotating Stars , 1999, astro-ph/9907433.

[51]  H. Janka,et al.  IS STRONG SASI ACTIVITY THE KEY TO SUCCESSFUL NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS? , 2011, 1108.4355.

[52]  K. Kotake,et al.  EFFECTS OF ROTATION ON STANDING ACCRETION SHOCK INSTABILITY IN NONLINEAR PHASE FOR CORE-COLLAPSE SUPERNOVAE , 2008, 0811.0651.

[53]  A. Mezzacappa,et al.  The Spherical Accretion Shock Instability in the Linear Regime , 2005, astro-ph/0507181.

[54]  Non-spherical core collapse supernovae. I. Neutrino-driven convection, Rayleigh-Taylor instabilities, and the formation and propagation of metal clumps , 2003, astro-ph/0302239.

[55]  H. Janka,et al.  A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE , 2012, 1202.0815.

[56]  H. Janka,et al.  HYDRODYNAMICAL NEUTRON STAR KICKS IN THREE DIMENSIONS , 2010, 1010.0167.

[57]  A. Mezzacappa,et al.  Stability of Standing Accretion Shocks, with an Eye toward Core-Collapse Supernovae , 2002, astro-ph/0210634.

[58]  E. Muller,et al.  An axis-free overset grid in spherical polar coordinates for simulating 3D self-gravitating flows , 2010, 1003.1633.