Top: Composite of SDO/AIA 171 Å image and SOHO/LASCO/C2 white-light coronagraph image. The longstanding observational gap is shown in dark grey. Bottom: Modeled acceleration profiles of torus instability CMEs, adapted from Török and Kliem (2007) Fig. 3. The different curves result from different background magnetic field decay index profile assumptions, with each higher acceleration peak corresponding to a larger decay index profile. Most of the acceleration occurs in the observational gap that SunCET fills.