  We present observations and modeling of the magnetic field configuration,
morphology, and dynamics of a large-scale, high-latitude filament eruption
observed by the Solar Dynamics Observatory. We analyze the 2015 July 9-10
filament eruption and the evolution of the resulting coronal mass ejection
(CME) through the solar corona. The slow streamer-blowout CME leaves behind an
elongated post-eruption arcade above the extended polarity inversion line that
is only poorly visible in extreme ultraviolet (EUV) disk observations and does
not resemble a typical bright flare-loop system. Magnetohydrodynamic (MHD)
simulation results from our data-inspired modeling of this eruption compare
favorably with the EUV and white-light coronagraph observations. We estimate
the reconnection flux from the simulation's flare-arcade growth and examine the
magnetic-field orientation and evolution of the erupting prominence,
highlighting the transition from an erupting sheared-arcade filament channel
into a streamer-blowout flux-rope CME. Our results represent the first
numerical modeling of a global-scale filament eruption where multiple ambiguous
and complex observational signatures in EUV and white light can be fully
understood and explained with the MHD simulation. In this context, our findings
also suggest that the so-called "stealth CME" classification, as a driver of
unexpected or "problem" geomagnetic storms, belongs more to a continuum of
observable/non-observable signatures than to separate or distinct eruption
processes.
