MHD Tomography Using IPS Observations

Details MHD Tomography Using IPS Observations MHD Tomography Using IPS Observations

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh31a0697h&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH31A-0697

Other

2124 Heliopause And Solar Wind Termination, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

We will present the tomography analysis method to derive three-dimensional solar wind structures from IPS observations using MHD simulation. By incorporating MHD simulation in tomography analysis, we can treat the nonlinear MHD interactions in solar wind and examine the spatial variation at the stream-stream interaction regions and spiral structure of IMF. Therefore, MHD tomography will improve the global solar wind structure derived from IPS measurement data. The method is based on the concept of the tomography, and the practical calculation is done as iteration procedure. At the first step of iteration, MHD simulation is carried out with given provisional boundary conditions, and the numerical three-dimensional solar wind is made. At the next step, the IPS observations are simulated in this three-dimensional solar wind. The differences between the actual IPS measurement and the numerically reproduced ones are traced back along streamlines onto the inflow boundary surface. Then, the velocity distribution on the boundary surface is modified so that the differences may be cancelled. For the MHD simulation, the boundary conditions of other solar wind parameters, density, temperature and magnetic field, are determined as follows. The density and temperature are determined by empirical relations to the velocity, and magnetic field is determined from the potential field approximation. The three-dimensional solar wind structures derived from this analysis were compared with the in-situ measurement data made by Ulysses and WIND, and good agreements were contained among them.

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