Modeling the Solar Wind in the Inner Heliosphere

Details Modeling the Solar Wind in the Inner Heliosphere Modeling the Solar Wind in the Inner Heliosphere

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh33a..07g&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SH33A-07

Computer Science

Performance

7599 General Or Miscellaneous, 7833 Mathematical And Numerical Techniques (0500, 3200), 7924 Forecasting (2722), 7959 Models

Scientific paper

One main effort of the Center for Integrated Space Weather Modeling (CISM) is to develop space weather models for the Sun-Earth chain. Among them is the Solar Wind model that gives a 3 dimensional description of the solar wind structures in the inner heliosphere. It is driven by daily NSO/SOLIS synoptic maps. We employ the Wang- Sheeley-Arge (WSA) algorithm to compute potential field solutions of the solar corona and derive inner boundary conditions for the ideal MHD code ENLIL. It in turn propagates the solar wind structures out to Earth and beyond. With this model we can describe the ambient solar wind at the three locations of the ACE and STEREO space crafts; we are also able to predict the plasma parameters for lead times of 1 to 5 days in 6 hour cadences. We report on validation efforts and prediction performance.

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