# Presentation: 357485

## DOE/SciDAC Supernova Science Center (SNSC)

- S.  Woosley (UCSC), A. Burrows (UA), C. Fryer (LANL), R. Hoffman (LLNL)+ 20 researchers

## Outline

- Institutions and Core Projects
- Codes, Simulation Capabilities, ISICS,  Platforms, Visualization
- List of Major Accomplishments to date
- Representative Scientific Results (graphics and animations)

## Slide 3

## Codes and Capabilities

- 2D/3D Anelastic hydro; spectral methods (+MHD) (Glatzmaier)
- VULCAN/2D Boltzmann/hydro (6D) (TOPS)
- Implicit Stellar Evolution (Kepler)
- 2D/3D Stellar Evolution
- 3D Hydro/diffusion (statistical methods)
- 2D/3D Thermonuclear combusion (APDEC)
- FLASH 2D/3D Hydro code
- 3D Monte Carlo radiation transport
- 3D Special relativistic hydro (GRBs)
- Nuclear Network solver(s)
- Visualization infrastructure at Arizona (Hariri)

## Main Computers and Platforms

- NERSC/seaborg
- ORNL/cheetah, eagle
- Beowulfs at LANL, UCSC, U.Arizona
- ASCI Q (LANL)

## Computational Nuclear Astrophysics

- Core-Collapse Supernovae (Grid-based & Statistical methods)
- Thermonuclear Supernovae (Type Ia)
- Gamma-Ray Bursts
- X-ray Bursts
- Stellar Convection simulations (2D/3D)
- World-class Nuclear Data Archive
- 1-,2-,3-D Radiation/Hydrodynamics
- Astrophysical Flame Physics
- Collaboratory- Vertically Integrated Nuclear Astrophysics: Stellar Evolution - Nucleosynthesis - Supernova Explosions - Light Curves

## Major Accomplishments

- First 3D Simulation of Core-Collapse Supernova (Diffusion)
- First 2D Boltzmann Rad/Hydro Simulation in Core Collapse: Multi-group, multi-angle
- First 3D Relativistic GRB Jet Calculation
- First Fully-Resolved 3D Rayleigh-Taylor  Nuclear Burning Study in Type Ia Supernova Context and 3D Simulation of Onset of Ignition
- First 1600-Species Nuclear Network Calculation for X-Ray Bursts
- Assembly of the World’s Most Comprehensive Nuclear Reaction Database
- 3D Stellar Convection simulations: sun, massive stars

## Hoffman (LLNL):  Nuclear Reaction Database

## Glatzmaier, 3D Anelastic MHD : Pulsar B-Fields?

## Tami Rogers UCSC

- Penetrative Convection

## Solar Convection Simulations: Anelastic Code with B-fields

- Solar Convection Simulations: Anelastic Code with B-fields

## Kuhlen et al.

- UCSC

- 3D Nuclear Burning

## Slide 13

## Type Ia Supernova Fusion Flame

-     ApJ (2004)

-  = 1.5 x 107 g cm-3

- Carbon mass fraction. Red is 50%.
-                                     Blue is zero

- _Nuclear fusion flame subject to_
- _both burning and the Rayleigh-Taylor_
- _instability._

- g

- Fuel

- Ash

- In collaboration with CCSE/LBL Group

- Type Ia Supernova Fusion Flame

## Slide 15

## Onion Skin Structure:  The Mote in the Eye of the Storm

## Fryer and Warren (LANL): First 3D Simulation

## Rayleigh-Taylor Mixing in a Type II Supernova

## Fryer, Warren, and Hungerford 2004: Radioactive Nickel

## University 

- University
-  of
- Arizona

## 11 Solar Masses

- Modest Rotation

## 11 Solar Masses

- Rapid Rotation

## 20 Solar Masses

- Modest Rotation
- Torus Formation

## Slide 24

## Perturbation Study

- Perturbation Study

## Slide 26

## VULCAN/2D Multi-Group, Multi-Angle, Time-dependent Boltzmann/Hydro (6D)

- Arbitrary Eulerian-Lagrangian (ALE); remapping
- 6 - dimensional   (1(time) + 2(space) + 2(angles) + 1(energy-group))
- Moving Mesh (FE)
- 2D multi-group, multi-angle, Sn (~150 angles),  implicit transport
- Axially-symmetric; Rotation
- Flux-conservative; smooth matching to diffusion limit
- Developing TOPS collaboration: solvers, pre-conditioners for transport (PETSc/Hypre) (needs speed)
- First 2D Boltzmann rad/hydro code in astrophysics

## VULCAN/2D

- Numerical
- Paradigm

## Color Map: Ye

- Vectors: Flux

- Multi-Group
- Multi-Angle
- Boltzmann
- Transport

- Livne, Burrows,
- et al. 2004, Ap.J.
- in press

## 2D MGFLD:  Core Collapse and Bounce; Entropy and Velocity Vectors

## 2D MGFLD: Entropy and Neutrino Flux (7.8 MeV)

## Slide 32

## SN1987A ?