Overview

Applications

• Grand Challenge Investigators
  • Simulations of Earth's Core and Mantle Dynamics
  • Turbulent Convection and Dynamos in Stars
  • Multiscale Modeling of Heliospheric Plasmas
  • Relativistic Astrophysics and Gravitational Wave Astronomy
• Grand Challenge Performance Milestones
• Guest Investigators
  • Earth and Space Sciences
  • Aerospace Sciences
• Inhouse Computational Scientists
  • Distributed Mission Simulation
  • Earth's Interior Modeling Grand Challenge Support
  • FPGA Implementation for On-Board Data Processing
  • High Performance Computing for Quantum Dot Modeling
  • Ocean Modeling Grand Challenge Support
  • Parallel Dimension Reduction for Remote Sensing Data

Testbeds

• SGI Final Report for ESS Round-2 (CRAY T3E at Goddard Space Flight Center)
• Hewlett-Packard X-Class Exemplar at Caltech/Jet Propulsion Laboratory (JPL)
• SGI Origin2000 at JPL
• System Performance Evaluation Project
• JPL Beowulf Activities
• Testbed Requirements Stated by Round-2 Investigators
  • Data for Lower, Medium, and Preferred Resolution Models
  • Mass Storage vs. CPU Requirements
  • Long Haul Network vs. CPU Requirements

System Software R&D

• Adaptive Mesh Refinement Software
  • The PYRAMID: Parallel Unstructured Adaptive Mesh Refinement Library
• The Beowulf Project
• Distributed Visualization Environments for ESS Applications
  • ParVox: A Parallel Volume Rendering System for Scientific Visualization
• ESS Kernels Templates for Software Portability and Reuse
  • Parallel Support Software for Matlab

Image: This visualization shows how a coronal mass ejection (CME) affects the Earth's magnetic field 94.5 hours after leaving the Sun. Stored energy and magnetic flux increase substantially in the planetary magnetic field; these effects can lead to power grid and satellite failures. The image is a snapshot from the first simulation to follow the Sun-to-Earth path of a CME, an event in which the star's outer atmosphere throws out a chunk of itself. Colors represent the electric current density. Solid lines trace the inner (red) and outer (green) boundary of the magnetic field, as defined by closed magnetic field lines. The simulation runs faster than real time, showing promise for better CME forecasts. Research: Tamas Gombosi, Darren De Zeeuw, Clinton Groth, Ken Powell, Quentin Stout, University of Michigan. Visualization: Darren De Zeeuw.

Authorizing NASA Official: James R. Fischer, ESS Project Manager
Editor and Web Curator: Jarrett S. Cohen, jarrett.cohen@gsfc.nasa.gov
Last Modified: August 31, 2000