MHD Code Optimizations and Jets in Dense Gaseous Halos

Volker Gaibler (), Matthias Vigelius (), Martin Krause () and Max Camenzind ()
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Volker Gaibler: Landessternwarte Königstuhl
Matthias Vigelius: University of Melbourne, School of Physics
Martin Krause: Astrophysics Group, Cavendish Laboratory
Max Camenzind: Landessternwarte Königstuhl

A chapter in High Performance Computing in Science and Engineering ’06, 2007, pp 35-48 from Springer

Abstract: Summary We have further optimized and extended the 3D-MHD-code NIRVANA. The magnetized part runs in parallel, reaching 19 Gflops per SX-6 node, and has a passively advected particle population. In addition, the code is MPI-parallel now — on top of the shared memory parallelization. On a 5123 grid, we reach 561 Gflops with 32 nodes on the SX-8. Also, we have successfully used FLASH on the Opteron cluster. Scientific results are preliminary so far.We report one computation of highly resolved cocoon turbulence. While we find some similarities to earlier 2D work by us and others, we note a strange reluctancy of cold material to enter the low density cocoon, which has to be investigated further.

Keywords: Galaxy Cluster; Radio Galaxy; Data Transfer Rate; Dense Shell; Galactic Wind (search for similar items in EconPapers)
Date: 2007
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DOI: 10.1007/978-3-540-36183-1_3

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