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January 9, 2007AAS/AAPT John M. Blondin NC State University Discovering the Complexity of Supernovae through 3D Simulations.

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Presentation on theme: "January 9, 2007AAS/AAPT John M. Blondin NC State University Discovering the Complexity of Supernovae through 3D Simulations."— Presentation transcript:

1 January 9, 2007AAS/AAPT John M. Blondin NC State University Discovering the Complexity of Supernovae through 3D Simulations

2 January 9, 2007AAS/AAPT

3 January 9, 2007AAS/AAPT We begin our story in 1572… ``On the 11th day of November in the evening after sunset, I was contemplating the stars in a clear sky. I noticed that a new and unusual star, surpassing the other stars in brilliancy, was shining almost directly above my head.’’ -- Tycho Brahe

4 January 9, 2007AAS/AAPT Again in 1604… Johannes Kepler observed a “stella nova” that became as bright as Jupiter, but faded away after a couple months.

5 January 9, 2007AAS/AAPT For 400 years there has not been a supernova in our Galaxy … we are still waiting! But, in a nearby galaxy not long ago (February 1987)…

6 January 9, 2007AAS/AAPT We can learn even more by looking at what is left hundreds of years later.

7 January 9, 2007AAS/AAPT Remnants of Supernova Explosions Relic Blastwave Spinning Neutron Star

8 January 9, 2007AAS/AAPT The iron core contains about 3 times the mass of our Sun, but it is roughly the size of our Earth. This iron core collapses under its own weight until it is small enough to fit inside Puget Sound. At this point the core is as dense as the nucleus of an atom and it cannot compress any further. The rest of the star ‘bounces’ off this hard core and explodes off into space???

9 January 9, 2007AAS/AAPT It all starts with core collapse…

10 January 9, 2007AAS/AAPT 1966 Colgate and White Neutrino-Driven prompt explosion 1985 Bethe and Wilson Shock reheating via neutrino energy deposition 1992 Herant, Benz, and Colgate Convective instability above neutrino-sphere The Supernova story has a long history of computational physics…

11 January 9, 2007AAS/AAPT The last decade has seen a great deal of interest in multidimensional effects: Convection with the proto- neutron star Neutrino-driven convection below the stalled shock Instability of the stalled shock All of these may operate together!

12 January 9, 2007AAS/AAPT First generation of 2D SN models hinted at a low-order asymmetry in the shock wave at late times (100’s of msec after bounce). Burrows, Hayes & Fryxell 1995

13 January 9, 2007AAS/AAPT REU Students, Summer 2000 Christine DeMarino Brett Unks Dana Paquin

14 January 9, 2007AAS/AAPT To investigate the dynamics of the stalled supernova shock, we consider an idealized problem:

15 January 9, 2007AAS/AAPT In One Dimension: Analytical: Houck & Chevalier (1992) presented a linear stability analysis. Numerical: Blondin et al. (2003) perturb SAS and watch the evolution. Pressure Perturbation Time -> Radius

16 January 9, 2007AAS/AAPT SN Code Verification This post-bounce model provides an opportunity to verify supernova codes against the results of a linear perturbation analysis. Houck and Chevalier 1992 Blondin and Mezzacappa 2005

17 January 9, 2007AAS/AAPT Spherical Accretion Shock Instability Blondin, Mezzacappa, DeMarino 2003, ApJ, 584, 971

18 January 9, 2007AAS/AAPT The SASI is a global acoustic mode: The spherical accretion shock acts as an acoustic cavity, with a trapped standing wave growing exponentially with time.

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20 January 9, 2007AAS/AAPT This initial SASI discovery with axisymmetric 2D simulations pointed to the obvious need for models in full 3D. Must move to 3D!

21 January 9, 2007AAS/AAPT Hurdles for Large-Scale 3D Simulation code Floating points Data output Data transport Visualization and analysis Not a problem Thank you DOE It works Does not work I can’t see!

22 January 9, 2007AAS/AAPT First Results: SASI Exists in 3D Without interactive access to the data, this was science in the dark! 3D Cartesian grid 100 Million zones 100’s of processors 100’s of GB in full run

23 January 9, 2007AAS/AAPT Science Begins with Data Scientific discovery is done with interactive access to data. Must have interactive access on a large-memory computer for analysis and visualization. Must have high bandwidth in accessing the data. Must have sufficient storage to hold data for weeks/months. Cray X1 Billion-cell simulation in 30 hours generates 4 terabytes Visualization platform Shared file system

24 January 9, 2007AAS/AAPT Interactive Visualization of TB Datasets A commodity linux cluster provides all the ‘must haves.’ Data is sliced into slabs and stored on local disks on the cluster nodes. EnSight Gold provides an easy visualization solution, including remote client-server operation and collaboration.

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36 January 9, 2007AAS/AAPT A non-rotating, spherically symmetric progenitor star can leave behind a neutron star spinning with a period of tens of milliseconds. SASI

37 January 9, 2007AAS/AAPT A Million Second Chandra View of Cassiopeia A “These are most likely due to jets of ejecta as opposed to cavities in the circumstellar medium, since we can reject simple models for the latter.” Hwang et. al. 2004

38 January 9, 2007AAS/AAPT Reverse shock Forward shock If the progenitor star possessed an asymmetric stellar wind (e.g., due to rotation), the supernova remnant driven into this relic wind would reflect the asymmetry of the wind. In this 2D simulation, the density in the progenitor wind is four times denser in the equatorial plane than at the poles.

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40 January 9, 2007AAS/AAPT  equator pole radius Never believe a jet in 2D…

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42 January 9, 2007AAS/AAPT Leading Shockwave Fast Ejecta Shocked Ejecta A “Jet” from a Spherical Supernova


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