Data assimilation of the solar wind in the inner heliosphere

Details Data assimilation of the solar wind in the inner heliosphere Data assimilation of the solar wind in the inner heliosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh51b2011t&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH51B-2011

Physics

Plasma Physics

[2162] Interplanetary Physics / Solar Cycle Variations, [2164] Interplanetary Physics / Solar Wind Plasma, [7833] Space Plasma Physics / Mathematical And Numerical Techniques

Scientific paper

The solar wind and the large-scale disturbances propagate in the inner heliosphere. They have significant effect on planetary environments. In order to understand their propagation and development in the simulation constrained by observations, we try data assimilation of the solar wind. We use three-dimensional magnetohydrodynamic (MHD) model of the solar wind with an inner boundary condition based on SOHO/MDI magnetic field data. As a preliminary method, solar wind velocity from interplanetary scintillation (IPS) observation is put into the simulation by weighting as a function of observation and system (model + inner boundary) errors. The latter is simulated to obtain as a function of heliospheric radius. The number of model grids is 41 (radial) x 6,912 (longitude and latitude) = 283,392, while that of observation data is 6,912 for the inner boundary and ~1,500 per one day from the IPS observation. Since the number of observation data is much smaller than simulation grid and the MHD system is mainly controlled by the inner boundary, the inner boundary model relating imaging observation and solar wind parameters is a key for the system. We show the present status of our approach for the solar wind data assimilation.

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