By Volker Gaibler, Max Camenzind (auth.), Wolfgang E. Nagel, Dietmar B. Kröner, Michael M. Resch (eds.)
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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Extra resources for High Performance Computing in Science and Engineering '09: Transactions of the High Performance Computing Center, Stuttgart (HLRS) 2009
Fig. 2 shows the accumulated CPU time and the total wall clock time as a function of the number of processors for a test run with 256 angular rays on the NEC machines SX-8 (8 CPUs per node) and SX-9 (16 CPUs/node) at HLRS and on the IBM Power6 575 (32 CPUs/node) at the Rechenzentrum Garching (RZG) of the Max-Planck-Gesellschaft. 85 could be obtained by using eight nodes instead of one, which corresponds to a parallel eﬃciency of more than 98%. 81 (parallel eﬃciency ≈ 95%). It should be pointed out, however, that the new MPI version is about 40% faster than the shared-memory version of the code even on a single Power 6 node, because it can better cope with the machine’s ccNUMA architecture.
694 (2009) 664–696 26. : Explosions of O–Ne–Mg cores, the Crab supernova, and subluminous type II–P supernovae. Astron. Astrophys. 450 (2006) 345–350 32 B. M¨ uller, A. -Th. Janka 27. : Toward Gravitational Wave Signals from Realistic Core-Collapse Supernova Models. Astrophys. J. 603 (2004) 221–230 28. : Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae. Astron. Astrophys. 496 (2009) 475–494 29. : Theory of core-collapse supernovae.
Hydrodynamic Simulations of Supernovae 27 instabilities like convection and a non-radial instability of the accretion shock front, the so-called SASI  were found to be of crucial importance for the explosion. Several other simulations covering the non-rotating case, and also employing the alternative stiﬀ nuclear equation of state of , have been performed as well (and others are still on the machines). A comparison of the diﬀerent models allows us to draw some interesting conclusions: A soft nuclear equation of state that causes a rapid contraction and a smaller radius of the forming neutron star and thus a fast release of gravitational binding energy, seems to be more favourable for an explosion.