Core-collapse Supernove through Cosmic Time...
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1 Core-collapse Supernove through Cosmic Time... Eric J Lentz University of Tennessee, Knoxville S. Bruenn (FAU), W. R.Hix (ORNL/UTK), O. E. B. Messer (ORNL), A. Mezzacappa (UTK), J. Blondin (NCSU), E. Endeve (ORNL), J. A. Harris (UTK), P. Marronetti (NSF), K. Yakunin (UTK)
2 Why study supernovae? Why do some stars explode? What leads up to the collapse? How does collapse of the core result in an explosion? SN 1987a in LMC Study exotic physics (nuclear matter, neutrinos, GR) and signals (neutrino, GW) Understand the generation of elements and their ejection.
3 Reviving stalled shock with neutrino heating standing accretion shock Adapted from Hillebrandt, Janka, & Müller, 2006, Sci. Am 295, 4, 42
4 Ingredients Matching the physical conditions to numerical inputs to reflect the physical fidelity of the system. Supernovae Pre-supernova stellar history General Relativity Fluid dynamics & Instabilities Equation of State Neutrino Transport Neutrino-matter interactions Simulations Stellar evolution models Full/Approximate/Newtonian Grids/Resolution/Symmetry Nuclear/Electron/Network Relativity/Moments/Spectral/ Ray-by-Ray Which ones are needed?
5 CHIMERA has 3 heads CHIMERA Spectral Neutrino Transport (MGFLD-TRANS, Bruenn) in Ray-by-Ray Approximation using modern neutrino opacities Shock-capturing Hydrodynamics (VH1 [PPM], Blondin) Nuclear Kinetics (XNet, Hix & Thielemann) Multipole gravity w/ Spherical GR correction Equations of State: Lattimer-Swesty (K=220 MeV) Cooperstein/BCK: ρ<10 11 g/cm 3 [Results: Bruenn et al 2006, 2009, 2013] Ray-by-Ray Approximation
6 Chimera numerics Multi-physics: operator split 540 (radial) x 180 (latitude) x180 (longitude) sphericalpolar grid w/ inner core (8 km) in spherical symmetry. 2-degree phi resolution Fixed d(cos theta) resolution (~8 deg at pole, to ~2/3 deg at equator) [fixed solid angle] Hydrodynamics: dimensional split, needs transposes Transpose: MPI_AllToAll on 180 sub-communicators MPI ranks (4050 XK7 nodes, 8 tasks/node, 2 OpenMP threads) Each MPI task computes one independent, transport solve using local data.
7 Dimension changes revival Key result from many previous studies: 1D does not explode, 3D may be favorable, or not. Chimera result: 15 M_sun star. 1D: Fails! 2D: short wait, rapid expansion 3D: longer delay, less vigorous? Shock Radius [km] D 1D 3D time after bounce [ms] Lentz et al., to be submitted shortly...
8 Comparison Images 23 C15-3D 200 ms km Text!""#$% 400 km C15-3D 300 ms 400 km!""#$% 400 km Lentz et al., to be submitted shortly...
9 More... C15-3D 300 ms 400 km Text!""#$% 400 km C15-3D 400 ms 400 km 400 km!""#$% Lentz et al., to be submitted shortly...
10 Shock Revival in 3D Yellow/green, Red: hot plumes; blue =~ shock Lentz et al., to be submitted shortly...
11 Plume sizes Preceding shock revival, plume size grows Radial velocity, 150 km radius shell Rising flows in red, sinking in blue Lentz et al., to be submitted shortly...
12 Resolution Initial work on Blue Waters: examine impact of resolution Low resolution make flows more viscous, terminates turbulent cascade, dissipates small features, etc Full resolution 2 degrees
13 Time to Develop Explosion 4 2D simulations covering mass range (12, 15, 20, & 25 solar masses). Shock revival at ~ ms, but full saturation of explosion much longer. Similar times required for quieting neutrino and GW signals. Explosion Energy [B] E + = Energy sum over positive energy zones E + ov = E+ + Overburden E + ov, rec = E+ + Nuclear recombination ov B12-WH07 B15-WH07 B20-WH07 B25-WH Post-Bounce Time [ms] (Bruenn et al. 2014, ApJ, subm.)
14 2D Comparison to Obs. Explosion energies (circles with arrows) fall in range of measured values from observed supernovae. Arrows indicate 1 sec. continued growth at ending rate SN 2009kr SN 2004et 0.1 SN 1993J Explosion Energy [B] SN 1993J SN 2004et SN 2004A SN 2004dj SN 2004 cs SN 2012aw SN 1987A SN 2012ec 56 Ni Mass [M ] SN 2004A SN 2005cs SN 1987A SN 2004et SN 2012aw SN 2004dj ZAMS Progenitor Mass [M ] ZAMS Progenitor Mass [M ] (Bruenn et al. 2014, ApJ, subm.)
15 Goals: PRAC project Similar coverage in mass for 3D simulations. Long runs to determine energy, signals, and ejecta properties. (1+ second) Develop library of simulations covert possible behaviors. Special goal: Compute nucleosynthesis (elemental & isotopic) yields of CCSNe and calibrate other models used to study the chemical evolution of galaxies.
16 2D Nucleosynthesis Recent measurements (Boggs et al. 2015, Science) show asymmetries in Ti-44 distribution in SN 1987A. Our simulations are also clearly asymmetric in Ti-44 (Harris et al, in prep.)
17 Prac details Design goals: 3 x 3 grid: 3 heavy element abundance levels (zero or primordial, low, solar) with 3 progenitor masses each. 1+ second simulation time 1-degree Yin-Yang grid (pole-free; less restrictive CFL time steps)
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