Authors: Provornikova, E. (JHU APL), Malanushenko, A. (NCAR, HAO), Vourlidas, A. (JHU APL), Gibson, S. (NCAR, HAO), Merkin, V.G. (JHU APL), C. N. Arge (NASA GSFC), M. Wiltberger (NCAR, HAO), K. Dalmasse (IRAP, Universite de Toulouse)

To improve our understanding of how the interaction of coronal mass ejections (CMEs) and the solar wind in the inner heliosphere (beyond 0.1 AU) affects resulting plasma and magnetic field variations when CME passes Earth, a physics-based model which accounts for the magnetic structure of CMEs and accurately describes the global solar wind background is required. We present the GAMERA-Helio model of the inner heliosphere driven by the WSA-ADAPT coronal model and coupled with the Gibson & Low model of a CME. We discuss boundary conditions treatment to emerge a magnetized CME into the solar wind at the GAMERA-Helio inner boundary. We analyze a subsequent evolution of a CME in different scenarios depending on a magnetic morphology of a CME bubble (detached spheromak, spheromak tethered to the origin and flux rope), location of emergence into the background implying weak or intense interaction with the solar wind stream interaction regions as well as an orientation of the 3D CME magnetic structure. We show how these different cases of CME-solar wind interactions give rise to a variety of geometric appearances in white light.