Authors: W. Manchester IV (University of Michigan), N. Sachdeva (University of Michigan), M. Ala-Lahti (University of Michigan), E. Kilpua (University of Helsink), S. Lata Soni (University of Michigan), Z. Huang (Universitty of Michigan), H. Chen (University of Michigan), A. Jivani (University of Michigan), B. van der Holst (University of Michigan), A. Szabo (NASA GSFC), M. Akhavan-Tafti (University of Michigan)

We investigate the formation and evolution of mesoscale structures that result from the interaction of a coronal mass ejection (CME) with the heliospheric current sheet imbedded in a Corotating interaction region. These structures dynamically form in our simulation of a CME performed with the Alfv ́en Wave Solar Atmosphere Model (AWSoM). With AWSoM, we first produce the background solar wind condition using synoptic magnetograms and properly defined photospheric Poynting flux. The CME is initiated from the originating active region with a Gibson-Low magnetic flux rope defined to match the observed event. With the use of high-resolution grids, we capture magnetic reconnection at the heliospheric current sheet and within/at the front boundary of ICMEs leading to the formation of meso-scale flux ropes containing sufficiently strong magnetic fields (~30 nT) to be geoeffictive. In this paper, we use these simulation results to demonstrate the capabilities of four probes of Space Weather Investigation Frontier (SWIFT) mission orbiting in tetrahedral orientation with 125 Re radial separation from L1 to sub-L1 location and 150 Re longitudinal/latitudinal separation at L1 location to observe the magnetic reconnection and evolution of small to-meso scale current sheet structure within the ICME.