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The Galactic Center black hole Sgr A* shows significant variability andflares in the submillimeter, infrared, and X-ray wavelengths. Owing to itsexquisite resolution in the IR bands, the GRAVITY experiment for the first timespatially resolved the locations of three flares and showed that a brightregion moves in ellipse-like trajectories close to but offset from the blackhole over the course of each event. We present a model for plasmoids that formduring reconnection events and orbit in the coronal region around a black holeto explain these observations. We utilize general-relativistic radiativetransfer calculations that include effects from finite light travel time,plasmoid motion, particle acceleration, and synchrotron cooling and obtain arich structure in the flare lightcurves. This model can naturally account forthe observed motion of the bright regions observed by the GRAVITY experimentand the offset between the center of the centroid motion and the position ofthe black hole. It also explains why some flares may be double-peaked whileothers have only a single peak and uncovers a correlation between the structurein the lightcurve and the location of the flare. Finally, we make predictionsfor future observations of flares from the inner accretion flow of Sgr A* thatwill provide a test of this model.

A Plasmoid Model for the Sgr A* Flares Observed with GRAVITY and Chandra