  Stealth coronal mass ejections (CMEs) are events in which there are almost no
observable signatures of the CME eruption in the low corona but often a
well-resolved slow flux rope CME observed in the coronagraph data. We present
results from a three-dimensional numerical magnetohydrodynamics (MHD)
simulation of the 1--2 June 2008 slow streamer blowout CME that Robbrecht et
al. (2009) called "the CME from nowhere." We model the global coronal structure
using a 1.4 MK isothermal solar wind and a low-order potential field source
surface representation of the Carrington Rotation 2070 magnetogram synoptic
map. The bipolar streamer belt arcade is energized by simple shearing flows
applied in the vicinity of the helmet streamer's polarity inversion line. The
flows are large scale and impart a shear typical of that expected from the
differential rotation. The slow expansion of the energized helmet streamer
arcade results in the formation of a radial current sheet. The subsequent onset
of expansion-induced flare reconnection initiates the stealth CME while
gradually releasing the stored magnetic energy. We present favorable
comparisons between our simulation results and the multiviewpoint SOHO-LASCO
(Large Angle and Spectrometric Coronagraph) and STEREO-SECCHI (Sun Earth
Connection Coronal and Heliospheric Investigation) coronagraph observations of
the preeruption streamer structure and the initiation and evolution of the
stealth streamer blowout CME.
