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Supercomputing in Astrophysics

Supercomputing in Astrophysics. April 20, 2006 Sang Min Lee KISTI Supercomputing Center. Three Basic Science Areas. Theory Mathematical modeling Various disciplines incorporated. Experimentation Verify theory Verify computations. Computation Provide input to what experiments to try

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Supercomputing in Astrophysics

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  1. Supercomputing in Astrophysics April 20, 2006 Sang Min Lee KISTI Supercomputing Center

  2. Three Basic Science Areas • Theory • Mathematical modeling • Various disciplines incorporated • Experimentation • Verify theory • Verify computations • Computation • Provide input to what experiments to try • Provide feedback to theoreticians • Play a role in bridge between the other areas

  3. Computation Science Area • Why Computation? • Numerical simulation fills a gap between physical experiments and theoretical approaches • Many phenomena are too complex to be studied exhaustively by either theory or experiments. • Besides complexity, many are too expensive to study experimentally, either from a hard currency or time point of view. • Computational approaches allow many outstanding issues to be addressed that cannot be considered by the traditional approaches of theory and experimentation alone. • In astrophysics, experiments may be impossible.

  4. Computational Scientist Requirements • Command of an applied discipline • Familiarity of leading edge computer architectures and data structures • Very good understanding of analysis and implementation of numerical algorithms • Familiarity with visualization methods and options.

  5. Supercomputing in Astrophysics • Why Supercomputing in Astrophysics? • Strong Interaction between matter and radiation • Ultimate goal of computation is to provide information that can be compared with observations • Very large amount of data, e.g., 5D(time, space, frequency) • Very huge dynamic range • Basically, need more than 20 orders-of-magnitude density dynamic range from a molecular clouds to stars • To study astrophysical phenomena, need supercomputing! • Multi-Physics • Magnetohydrodynamics, self-gravity, radiation transport, rotation, numerical relativity, turbulence, etc…… Astrophysical supercomputing are challenging! Rapid development of the computer technology opens this.

  6. KOREA Supercomputing Resources (KISTI) Cray 2S[1호기] Cray T3E NEC SX-5[3호기 1차] NEC SX-6[3호기 2차] TeraCluster (1997. 6. ~ 2003. 1.) 115GFlops (2001. 5. ~ 현재) 80GFlops (2003. 2. ~ 현재) 160GFlops ( 2003. 12 ~ 현재) 2,850GFlops 1988 1993 1997 2000 2001 2002 2003 2006 2GFlops 16GFlops 131GFlops 242GFlops 306GFlops 8,000GFlops 1,407GFlops 40TFlops HP GS320 HPC160/320 PC Cluster 128node IBM p690[3호기 1차] IBM p690+[3호기 2차] Cray C90[2호기] (2000. 5. ~ 2005. 11) 111GFlops (2001. 12. ~ 현재) 435.2GFlops (2002. 1. ~ 현재) 665.6GFlops (2003. 7. ~ 현재) 3,699.2GFlops (1993. 11. ~ 2001. 5.) 16GFlops

  7. Some Grand Challengesin KOREA • Large-Scale Structure Simulations (Park & Kim) • Verifying cosmological standard model • IBM p690 128CPUs 90days 1Billion particles(900GByte) From past to now Structures in Current Universe

  8. Some Grand Challenges in KOREA • Large-Scale Simulation on Cluster of Galaxies (Ryu et al.) • Studying cosmic shocks • 1,0243 simulation, IBM p690 32 CPUs, 60 days

  9. Some Grand Challenges in KOREA • Galactic Large-Scale Structure Simulations (Seo et al.) • 3D GMHD 256×512×256 grids, IBM p690 8 CPUs 4days • highly optimized MHD code, highly accurate gravity solver • considering external and self gravities

  10. Some Grand Challenges in KOREA (Planed) • Relativistic Flows (KOREA Center for Numerical Relativity) • Numerical simulation of magnetized cosmic jets • General relativity MHD(GRMHD) simulation of accretion disks • Numerical Relativity (NR) in Gravitational wave astronomy M87 Cosmic Jet Relativistic Jet Simulation GRMHD of accretion disk NR simulation

  11. Some Grand Challenges in Canada • The Merger of the Milky Way and Andromeda Galaxies (Dubinski, CITA) • Blue Horizon: 1,152 processor IBM SP3 at the SDSC 2001 • Each galaxy is described with 100 M particles.

  12. Numerical Astrophysics in the Past 70 Years • 1935: Stellar structure • with polytrope and the Lane-Emden equation • Adding machine (1Flop, ~10 Bytes) • 1965: Moore’s law • 1970: Stellar collapse • with 2D MHD code, 40×40 grid • CDC (1-10 Mflops, 1MByte) - 106~7 times improvement • 2003: Moore’s law is forever but ‘Hwang’s law’ • 2006: Stellar collapse, disks, jets, etc • With 3D MHD code, 103×103×103 grid • various supercomputers (10-300 TFlops, 100TByte) - 106~7 times improvement

  13. Numerical Astrophysics in the Next 34 Years • 2040 (34 years from now) • Hardware: 106~7 times improvement • 0.1 ~ 1 ZettaFlops machine • Explicit, time-dependent simulations, more resolution, more time steps • Software: AMR, implicit multi-time-scale technique • AMR used in other higher-order techniques • Seamless star evolution, BH formation & collisions

  14. Thank you for attention.

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