1) PI: Tamas Gombosi / University of Michigan - The Comprehensive Corona and Heliosphere Model (CCHM)
Next Team Meeting:
2) PI: Jon Linker / SAIC - A Next-Generation Model of the Corona and Solar Wind
Next Team Meeting:
3) PI: Leonard Strachan / Smithsonian Astrophysical Observatory - Quantitative Validation and Assessments of Solar/Heliospheric 3D Model Codes Using Empirical Data from Remote-Sensing and In Situ Measurements
Next Team Meeting:
The second strategic goal is a 3D time-dependent model that provides the structure and properties of the slowly varying corona and the ambient solar wind.
Expected features of such a model include:
- A 3D quantitative description of the structure and properties of the large scale corona and heliosphere at any given instant in time;
- The ability to use both presently available and forthcoming line-of-sight (LOS) photospheric magnetic field data from ground- and space-based solar observatories as input;
- User-friendly interfaces and graphics for runs on demand by the general research community;
- The flexibility for quick-turn-around runs; and
- Ability to deliver a working version, with rigorous evaluation and validation procedures, to the CCMC and/or other NASA LWS or NSF centers within three to five years.
Desirable features of such a model include:
- The use of vector magnetic field observations as input;
- Predictions of time dependent solar wind parameters at point or object (Earth, Mars, spacecraft) in space;
- Ability to initiate simple transients (e.g., pressure pulses); and
- Modularity sufficient to include routines containing new or more sophisticated physics (e.g., improved energetics, erupting CMEs).
