<h2>Chihiro Tao Solar Wind Model Data at AMDA</h2>
These data sets are the simulation outputs of solar wind variations observed
near the Earth and propagated to the different destinations using 
a 1-dimensional 2-component (radial & azimuthal) 
magnetohydrodynamic (MHD) model. 
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The model code is based on the
<a href="http://www.astro.phys.s.chiba-u.ac.jp/netlab/astro/index2-e.html" 
TARGET=_BLANK>Coordinated Astronomical Numerical Software (CANS) by JST</a>.
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Model details, evaluations compared with observation data, and limitations are described in
<a href="http://onlinelibrary.wiley.com/doi/10.1029/2004JA010959/abstract" TARGET=_BLANK> 
Tao et al. 2005, J. Geophys. Res., 110, A11208, doi:10.1029/2004JA010959</a>
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Solar wind propagation was calculated with several inputs : <i>input_OMNI, input_Stereo-A, input_Stereo-B</i>  
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Note an important parameter - <b>ephemeris/dPhi</b> - which could be considered as quality flag and 
presents an angle  <i><b>SOURCE</b>(Earth,Stereo-A,Stereo-B)-<b>SUN</b>-<b>TARGET</b>(Mars,Jupiter,Saturn)</i>
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For unknown points or other requests, please contact Chihiro Tao (<i>chihiro.tao@irap.omp.eu</i>).