Supernovae. Tomek Plewa. ASC Flash Center, University of Chicago. Konstantinos Kifonidis, Leonhard Scheck, H.-Thomas Janka, Ewald Müller
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1 Supernovae Tomek Plewa ASC Flash Center, University of Chicago Konstantinos Kifonidis, Leonhard Scheck, H.-Thomas Janka, Ewald Müller MPA für Astrophysik, Garching FLASH, Nov
2 Outline Non-exotic neutrino-driven supernovae Rayleigh-Taylor mixing in normal Type II Hydrogen-free case of Type Ib Bits from the Labs Conclusions FLASH, Nov
3 Non-exotic neutrino-driven supernovae Rayleigh-Taylor mixing in normal Type II Hydrogen-free case of Type Ib Bits from the Labs Conclusions FLASH, Nov
4 Introduction Most core collapse supernovae are aspherical. Evidence for strong 56 Ni mixing: light curves, emission line profiles, early detection of gamma rays in SN 1987A,... Mixing is currently the only source of detailed observational information on explosion mechanism. 2D/3D hydrodynamic models required to link theory to observations! FLASH, Nov
5 Starz! FLASH, Nov
6 The neutrino driven mechanism Complex multidimensional flow with heating and cooling (Chandrasekhar, Herant, Foglizzo, plus lots of numerical simulations done in the US, Europe, and Japan). Possibly offers the most conservative hydrodynamic mechanism for kicks (requires high-quality hydrodynamic models). FLASH, Nov
7 Anatomy of an exploding star FLASH, Nov
8 2D hydrodynamic models Progenitor: 15 Msol blue supergiant (WPE 88) Parameterized neutrino luminosities (inner boundary at neutrino sphere, no transport) PPM hydro solver + 14 isotope nuclear network Selfgravity Block Structured Adaptive Mesh Refinement Relatively simple, inexpensive physics 3072 ( per R * ) x 768 zones, remapping FLASH, Nov
9 Non-exotic neutrino-driven supernovae Rayleigh-Taylor mixing in normal Type II Done before, why to redo it? Hydrogen-free case of Type Ib Bits from the Labs Conclusions FLASH, Nov
10 Neutrino-driven Convection FLASH, Nov
11 Entropy, evolution up to 1 s FLASH, Nov
12 Numerical sanity Naturally seeded RT phase. FLASH, Nov
13 Model assumptions Same total core emission, longer timescale. FLASH, Nov
14 Long-term convection Short wavelength modes are filtered out; m=0,l=1 survives. FLASH, Nov
15 Long-term convection in 3D Confirms 2D results (but extremely expensive to obtain). FLASH, Nov
16 Pulsar kicks Observed bi-modal distribution and amplitudes recovered. FLASH, Nov
17 Post-bounce 1D evolution Shock revival after ~300 ms. FLASH, Nov
18 Basic 1D structure Reverse shock forms after ~300 ms. FLASH, Nov
19 Composition of 1D model Layered, highly discontinuous, several material interfaces. FLASH, Nov
20 Origins of mixing: I Density and pressure gradients of opposite signs. FLASH, Nov
21 Origins of mixing: II Shock speed deceleration. FLASH, Nov
22 Rayleigh-Taylor growth rates Long-term growth at He/H. FLASH, Nov
23 Log (density), 4 s post bounce Shock O/He interface Si/O interface Ni56 rich layers FLASH, Nov
24 Log (density), 10 s FLASH, Nov
25 Log (density), 20 s Compression of metal core Reverse shock FLASH, Nov
26 Density + elements, 50 s FLASH, Nov
27 Density + elements, 300 s FLASH, Nov
28 Density + elements, 1170 s O16 Ni56 Si28 FLASH, Nov
29 Log (density), 1620 s H/He interface He "wall" Reverse shock FLASH, Nov
30 Log (density), 3000 s FLASH, Nov
31 Log (density), 5000 s FLASH, Nov
32 Log (density), s FLASH, Nov
33 Log (density), up to 20,000 s FLASH, Nov
34 Velocity distributions, Type II model SN 1987A Kifonidis et al. (2004) FLASH, Nov
35 Model ejecta AD2005 Kifonidis et al. (2006) FLASH, Nov
36 Non-exotic neutrino-driven supernovae Rayleigh-Taylor mixing in normal Type II Hydrogen-free case of Type Ib Bits from the Labs Conclusions FLASH, Nov
37 Log (density), Type II model, 1620 s H/He interface He "wall" Reverse shock FLASH, Nov
38 Log (density), Type Ib model, 1600 s FLASH, Nov
39 Velocity distributions, Type Ib model FLASH, Nov
40 Mixing and spectra of Type Ib SN This work Model 4B of Eastman & Woosley (1997) FLASH, Nov
41 Non-exotic neutrino-driven supernovae Rayleigh-Taylor mixing in normal Type II Hydrogen-free case of Type Ib Bits from the Labs Conclusions FLASH, Nov
42 NLUF Supernova Rayleigh-Taylor Study RM / RT instability-driven transition to turbulence in a planar system at a diagnosable scale. t = 13ns t = 25ns t = 37ns Experiment geometry Au Grid Kifonidis, Plewa, Janka, & Mueller, 2000, Ap. J. 531, L123 Laser 50 mg/cm 3 CRF Re ~ Is this turbulence? interface Be tube Be shield 1.4 g/cm 3 polyimide FLASH, Nov Harry Robey et al., LLNL 42
43 Shock-cylinder cylinder interaction Problem is well-suited to AMR. Size of equivalent uniform 3D grid: 1280 X 256 X 256. AMR allows 6-level simulation to be completed in ~1000 node-hours on frost.llnl.gov. Breaking symmetry: variation in SF6 concentration in cylinder with depth. Visualizations allows to observe change in cylinder density with height, from bottom to top, at late stage. Chris Tomkins et al., LANL FLASH, Nov
44 Conclusions Neutrino driven convection seeds Rayleigh-Taylor instability at Si/O and O/He-interfaces. Complex post-shock flow, difficult to model, rich in surprises, not yet fully understood. Final 56 Ni velocities small compared to SN 1987A. The cause: hydrodynamic deceleration at He/H interface! Perhaps non-standard" progenitor models, additional physics (rotation or MHD effects), or possibly simply better treatment of currently considered physics required for SN 1987A. Promising mechanism to explain Type Ib spectra and light curves! FLASH, Nov
45 Discussion FLASH, Nov
46 FLASH, Nov
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