A model for an NIR flare with an accompanying sub-mm dip compared to the data from July 20 (see caption of Fig. 5). Compared to the sub-mm-radio SED shown in black square/diamonds, it can be seen that the flux of the sub-mm dip (red star) is lower than the typical sub-mm flux. The dashed lines show a toy model for the flare, in red, as well as for the “missing” sub-mm flux, in blue. The blue solid line shows the quiescent model of Yuan et al. (2003), and the red solid line represents the same model but with the “missing” sub-mm flux subtracted and the flare emission added. This particular figure shows the decreasing magnetic field case: to prevent overproduction of synchrotron emission from the accelerated population the magnetic field decreases from B = 30 G to B = 14 G. The spectrum for the case of the loss of electrons is very similar.