AAS 204th Meeting, June 2004
Session 67 Solar Input to the Heliosphere
SPD Topical Session, Wednesday, June 2, 2004, 2:30-4:00pm, 4:15-6:00pm, 704/706

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[67.02] MHD Simulation Model of the Interplanetary Disturbance Propagation Following the Flare of 2002 April 17

K. Hayashi, X.P. Zhao, Y. Liu (Stanford University)

An M2.6-class flare occurred on 2002 April 17. An associated halo coronal mass ejection (CME) was observed by SOHO/C3 and an ejecta and a transient shock were measured near the Earth after about 50 hours. We present three-dimensional time-dependent MHD simulation results of the interplanetary disturbance propagation for this event.

The simulation model is divided into three parts. In the first part, the steady trans-Alfvénic solar wind on April 17 was simulated by using the photospheric magnetic field map made at Wilcox Solar Observatory at Stanford University. This simulation was done for the regions r < 30 Rs. In the second part, using the solar wind map at 30 Rs, the steady super-Alfvénic solar wind at 30 Rs < r < 1 AU was calculated. In the last part, the numerical perturbations imitating the CME were given to this numerically obtained steady solar wind and the interplanetary disturbance propagation at 30 Rs r < 1 AU was simulated as the response of the solar wind to the perturbation. In this study, as input to the steady solar wind, the propagation velocity and the angular width of the halo CME at 30 Rs are determined using the cone model [Zhao et al., JGR, 107, A10, 2002].

The simulated solar wind variables were sampled at the position of the Earth, and compared with the nearby-Earth measurement data. We used the OMNI database at NSSDC/NASA for this comparison. The arrival time of the interplanetary shock to the Earth agreed well with the nearby-Earth measurement, within a few hours difference.

The data used in this simulation model can be prepared within several hours after a CME/flare event occurs. This will be useful for the field of space weather prediction studies.

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