Comparative Analyses of Two Extremely Fast CMEs Induced Shocks using A H3DMHD Model

During the last two decades, spacecraft recorded several extremely fast Coronal Mass Ejections (CMEs) which have resulted in severe geomagnetic storms. Here, we will report results from a comparative study of two extremely fast CME events: one on 29 October 2003 (Halloween 2003 epoch) and the other on 23 July 2012. Both shock events reached 1 AU within ~20 hours. We employed a global three-dimensional (3D) magnetohydrodynamics (MHD) simulation model (H3DMHD, Wu et al. 2007, JGR) to study these two events and compared the results with observations (e.g., 1 AU in-situ data, and coronal images from SOHO/LASCO or STEREO/ SECCHI). It was found that: (i) The peak temperature, velocity, and density of the solar wind for the shock/ICME event are 2 x 107 K, 2500 km s-1, and 35 cm-3, respectively. (ii) The peaks of magnetic field (B) are ~60 and 110 nT for the event on 29 October 2003 and 23 July 2012, respectively. Solar wind densities behind the shocks are extremely low which are due to rarefaction of the interplanetary shocks' propagation. We will discuss this issue in the presentation. Simulations are vastly improved and forecasting arrival times should be done as noted in real time by Zhou and Dryer (Space Weather Quarterly, 2014) review, but CME and B therein is still a major challenge for storm prediction.