- Conference date: 17-31 June 2002
- Location: Pisa (Italy)
We present the tomography analysis method using MHD simulation code to derive three‐dimensional solar wind structures from IPS observations. By incorporating MHD simulation, this new tomography method, hereafter called MHD tomography, can treat the nonlinear MHD process in solar wind and will improve the result of the reconstruction of global solar wind structure from IPS measurement data. 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 discrepancy 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 reduced. The modified boundary distribution is used in the next iteration, and the iteration is continued until the three‐dimensional solar wind structure matching the LOS‐integrated IPS observational data is obtained. The basic result of this analysis is shown, and the possible applications of this MHD‐based and observation‐based solar wind are demonstrated.
- Solar wind
- Surface boundary
- Boundary value problems
Y. K. Semertzidis, M. Aoki, M. Auzinsh, V. Balakin, A. Bazhan, G. W. Bennett, R. M. Carey, P. Cushman, P. T. Debevec, A. Dudnikov, F. J. M. Farley, D. W. Hertzog, M. Iwasaki, K. Jungmann, D. Kawall, B. Khazin, I. B. Khriplovich, B. Kirk, Y. Kuno, D. M. Lazarus, L. B. Leipuner, V. Logashenko, K. R. Lynch, W. J. Marciano, R. McNabb, W. Meng, J. P. Miller, W. M. Morse, C. J. G. Onderwater, Y. F. Orlov, C. S. Ozben, R. Prigl, S. Rescia, B. L. Roberts, N. Shafer‐Ray, A. Silenko, E. J. Stephenson, K. Yoshimura and EDM Collaboration
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