Authors: Nada Al-Haddad (SSC, UNH), Noé Lugaz (SSC, UNH)

Magnetic field structure of Coronal Mass Ejections has been often thought of as accurately represented by a highly twisted flux rope structure that extends from the solar surface into the corona. This paradigm has been proposed as a mean to explain early observations of CMEs, specifically magnetic clouds that exhibit a smooth rotation in their magnetic field. Models that have been developed based on this paradigm have been shown to not adequately fit the magnetic field. Plentiful studies since the early discovery of CMEs have demonstrated that the magnetic field structure is far more complex than a “simple” highly twisted flux rope (which can represent a local portion of the global structure, or the structure at a given time), and that 1D measurements of CMEs are not sufficient to provide a sense for what the global magnetic structure of CMEs is like. This work presents a representation of the three dimensional magnetic structure of CMEs based on 40+ years of studies of the different aspects of CMEs from their eruptions and throughout their propagation.