## 1. Introduction

[2] Because the dynamics of the solar wind can be well described by the magnetohydrodynamics (MHD) equations, two- and three-dimensional MHD simulation has been widely used to determine the global structure of solar wind and the temporal evolution of the transient phenomena such as the interplanetary disturbance propagation. For the study of the interplanetary disturbance, many MHD simulation studies give the numerical perturbation mimicking the transient event such as coronal mass ejection (CME) to the quiet background solar wind to induce the interplanetary disturbance event [e.g., *Odstrcil et al.*, 2004]. For this model approach, it is important to prepare realistic multi-dimensional background solar wind and the perturbation parameters that well represent the reality. Therefore, it is preferable if the simulated MHD variables are set up using the measurement data.

[3] There are several approaches to obtain the global three-dimensional structure of the quiet background solar wind. One of them is to simulate the trans-Alfvénic solar wind and solar corona starting from the solar surface, or photosphere, on which the observation-based magnetic field can be given as the boundary condition [e.g., *Linker et al.*, 1990; *Usmanov and Dryer*, 1995]. This approach must be orthodox, however, sophistication of the coronal heating and solar wind acceleration model is required so that the realistic solar wind solution will be obtained. Another approach is to use the interplanetary radio scintillation (IPS) measurement data and analysis methods [e.g., *Jackson et al.*, 1998; *Kojima et al.*, 2001] that can reconstruct the solar wind structures at *r* ≥ 25*R*_{s}. The MHD-version of the IPS tomography analysis [*Hayashi et al.*, 2003] can numerically reconstruct the three-dimensional steady MHD solution of the co-rotating solar wind from the line-of-sight integrated IPS measurement data. Because the solar wind observable by IPS measurement represents the consequence of the solar wind heating and acceleration process, it is a suitable choice to use the IPS-based MHD solution as the background solar wind in which the numerical interplanetary disturbance will propagate.

[4] In order to parameterize the CME structure, the Cone-model was proposed by *Zhao et al.* [2002] and improved by *Xie et al.* [2004] as the inversion method to determine the kinematic and geometric parameters of CME from the line-of-sight coronagraph data. This analysis method can determine the direction, the latitudinal and longitudinal angular widths, and the speed of CME by fitting the five parameters of the Cone-model geometry to the observation. They used the LASCO/C3 observation data at 5*R*_{s} < *r* < 23*R*_{s}. In addition, the Cone-model can derive the position of CME as a function of time; therefore, the time at which the CME will pass the reference distance can be estimated. The Cone-model in this way can provide the parameters needed to start MHD simulation of interplanetary disturbance.

[5] In this study, we will present the MHD simulation that uses the MHD-version of IPS tomography and the Cone-model. A new feature of this simulation is that both three-dimensional structure of the quiet solar wind and the characteristics of the interplanetary disturbance are determined from the measurements. Therefore, without treating the complex coronal dynamics, the simulation setup can be well prepared. We chose a period, mid-April 2002, during which two halo-CME events occurred. By choosing this period, we can additionally examine how the second event will propagate in the solar wind distributed by the first event.