Coronal Mass Ejections (CMEs) Induced Shock Formation and Properties

It has been recognized that solar energetic particles (SEPs) are accelerated at interplanetary shocks from the point of their formation in the lower corona to 1 A.U. and beyond. In this study, we will investigate the formation and propagation of induced shocks from the inner corona to 1 A.U. using a CME three-dimensional, axisymmetric (i.e. 2.5-D) magnetohydrodynamic (MHD) code. A well-studied CME event (1997 January Sun-Earth Connection Event) is used as a baseline to match the solar wind conditions measured at 1 AU (WIND data) to model CME driven shocks. The properties of the shock as a function of distance and latitude from the Sun up to 1 A.U. will be presented. Also, the geoeffective parameters are computed using disturbed solar wind properties.