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We present observations and modeling of the magnetic field configuration,morphology, and dynamics of a large-scale, high-latitude filament eruptionobserved by the Solar Dynamics Observatory. We analyze the 2015 July 9-10filament eruption and the evolution of the resulting coronal mass ejection(CME) through the solar corona. The slow streamer-blowout CME leaves behind anelongated post-eruption arcade above the extended polarity inversion line thatis only poorly visible in extreme ultraviolet (EUV) disk observations and doesnot resemble a typical bright flare-loop system. Magnetohydrodynamic (MHD)simulation results from our data-inspired modeling of this eruption comparefavorably with the EUV and white-light coronagraph observations. We estimatethe reconnection flux from the simulation's flare-arcade growth and examine themagnetic-field orientation and evolution of the erupting prominence,highlighting the transition from an erupting sheared-arcade filament channelinto a streamer-blowout flux-rope CME. Our results represent the firstnumerical modeling of a global-scale filament eruption where multiple ambiguousand complex observational signatures in EUV and white light can be fullyunderstood and explained with the MHD simulation. In this context, our findingsalso suggest that the so-called "stealth CME" classification, as a driver ofunexpected or "problem" geomagnetic storms, belongs more to a continuum ofobservable/non-observable signatures than to separate or distinct eruptionprocesses.

Modeling a Coronal Mass Ejection from an Extended Filament Channel. I. Eruption and Early Evolution