High Performance Computing in Science and Engineering '09 (PDF)
Transactions of the High Performance Computing Center, Stuttgart (HLRS) 2009
(Sprache: Englisch)
At the end of the year 2008, we have seen a strategic step towards a funct- ning HPC infrastructure on Tier-0 level in Germany. Based on an agreement ( Verwaltungsabkommen") between the Federal Ministry of Education and " Research (BMBF) and the state...
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At the end of the year 2008, we have seen a strategic step towards a funct- ning HPC infrastructure on Tier-0 level in Germany. Based on an agreement ( Verwaltungsabkommen") between the Federal Ministry of Education and " Research (BMBF) and the state ministries for research of Baden-Wurttem- ¿ berg, Bayern, and Nordrhein-Westfalen, a budget of overall 400 Million Euro had been allocated - equally shared between federal and state authorities in a ?ve year time frame - to establish the next generation of HPC systems at the Gauss Centre for Supercomputing (GCS) - consisting of the three nat- nal supercomputing centres HLRS (Stuttgart), NIC/JSC (Julich), and LRZ ¿ (Munich). As part of that strategic initiative, in May 2009 already NIC/JSC has installed the ?rst phase of the GCS HPC Tier-0 resources, an IBM Blue Gene/P with roughly 300. 000 Cores, this time in Julic ¿ h, With that, the GCS provides the most powerfulhigh-performance computing infrastructure in - rope already today. HLRS and its partners in the GCS have agreed on a common strategy for the installation of the next generation of leading edge HPC systems. Over the next few years, HLRS and LRZ as the other two GCS centers will upgrade their systems accordingly. The plan is to have a Tier-0 HPC system within GCS operating at any time in this ?ve year period. Asanintermediatestep,HLRShasreplacedmostoftheirNECSX-8nodes by the NEC SX-9/12M192, a system with roughly 20 TFLOPs peak.
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"Numerical Models for Emission Line Nebulae in High Redshift Radio Galaxies (S. 3-4)Summary. We examine models for line-emitting gas nebulae around powerful radio galaxies in the early universe. The models assume that either the emitting gas clouds are embedded in the shocked ambient gas and driven outwards with it or that they are created and sustained by multi-phase turbulence in the jet cocoon. For this, we perform jet simulations with realistic density contrasts on large scales and on typical activity time scales of several ten million years. The employed magnetohydrodynamics code NIRVANA has been optimized for the NEC SX machines in the previous years and now runs very e?ciently on the SX-6 and SX-8, allowing us simulations both in axisymmetry and full three dimensions. Future simulations on the SX-9 will bene?t signi?cantly from the increased number of shared memory processors per node for the axisymmetric runs, where an MPI-parallelization is generally ine?cient for our setup due to communication overhead.
1 Introduction
Extragalactic jets are amongst the most spectacular phenomena in astrophysics: These collimated beams of dilute but highly energetic plasma are formed in the environs of active black holes, on scales of milliparsecs3 with speeds very close to the speed of light, and propagate far outwards, eventually leaving the galaxy and pushing through the intergalactic gas at hundreds or even thousands of kiloparsecs.
Over these more than seven orders of magnitude in length, they remain collimated and deposit a large fraction of their huge kinetic energies of ∼ 1039 watts on the ambient gas. Yet, due to their low densities relative to the gas in galaxy cluster, they expand only slowly and reach their largest sizes only after several tens of millions of years. While these objects have been discovered already more than 50 years ago as double radio sources, only improving observational
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techniques made it possible in the 1970s and 1980s to realize the underlying physical mechanism of supersonic beams carrying large amounts of kinetic energy.
Jets do not only occur in the local universe, but also at high redshifts [13], corresponding to a time only some billion years after the big bang, when galaxies were still actively forming. At redshifts z > 0.5, radio galaxies often show luminous emission regions extending far beyond the galaxy itself, which are aligned with the radio source (“alignment e?ect”). These gas nebulae consist of an outer quiescent component, usually outside the radio structures, and an inner component with strongly distorted kinematics and clumpy and irregular structure [15]."
Jets do not only occur in the local universe, but also at high redshifts [13], corresponding to a time only some billion years after the big bang, when galaxies were still actively forming. At redshifts z > 0.5, radio galaxies often show luminous emission regions extending far beyond the galaxy itself, which are aligned with the radio source (“alignment e?ect”). These gas nebulae consist of an outer quiescent component, usually outside the radio structures, and an inner component with strongly distorted kinematics and clumpy and irregular structure [15]."
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Bibliographische Angaben
- Autor: Michael Resch
- 2010, 2010, 551 Seiten, Englisch
- Herausgegeben: Wolfgang E. Nagel
- Verlag: Springer-Verlag GmbH
- ISBN-10: 3642046657
- ISBN-13: 9783642046650
- Erscheinungsdatum: 28.04.2010
Abhängig von Bildschirmgröße und eingestellter Schriftgröße kann die Seitenzahl auf Ihrem Lesegerät variieren.
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Pressezitat
Aus den Rezensionen:“Obwohl auch aus finanziellen Gründen eigentlich auf einen engen Kreis von Forschern beschränkt, ist die Simulation mit Supercomputern bzw. deren Resultate kaum mehr aus unserem Alltag wegzudenken - Stichwort numerische Wettervorhersage. ... Ein wissenschaftliches Buch, das den aktuellen Stand des vielfältigen Einsatzes von Supercomputing in Deutschland präsentiert.“ (in: Bulletin SEV/VSE, February/2010, S. 87)
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