File:Massive Star Supernovae Explosions.jpg
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English: Three Dimensional Radiation Hydrodynamics Calculations of Massive Star Supernovae Explosions
The DJEHUTY stellar evolution code was used to calcuate the explosion of SN 1987A model in three dimensions, including the production and distribution of radioactive Ni-56, which powers most of the light emanating after the first few days. 2x1051 ergs of energy were placed within the innermost 150 km of the model to initiate the explosion. The initial density field was perturbed 10% to allow instabilities to grow, which is mandated by observations. Self-gravity was run in the spherical approximation but was centered on a self-consistently calculated center of mass. The simulation encompassed the whole star, contained 11 million cells, and was run on 512 processors of LLNL's Frost supercomputer for 36 hours. The resulting dataset was approximately 2 terabytes. |
| Date | Updated: November 8, 2007 |
| Source | Visualizations that have been created with VisIt. at wci.llnl.gov |
| Author | UCRL |
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This work is in the public domain in the United States because it is a work prepared by an officer or employee of the United States Government as part of that person’s official duties under the terms of Title 17, Chapter 1, Section 105 of the US Code.
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| current | 00:31, 11 July 2008 | | 500 × 400 (39 KB) | Mdd (talk | contribs) | {{Information |Description={{en|1=Three Dimensional Radiation Hydrodynamics Calculations of Massive Star Supernovae Explosions The DJEHUTY stellar evolution code was used to calcuate the explosion of SN 1987A model in three dimensions, including the prod |
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