Fig. 4
From: Transient rotation of photospheric vector magnetic fields associated with a solar flare
Intensity profiles of the NIR line at 1.56m during the flare a Stokes I component taken at 17:32:35 UT. The intensity is normalized to the maximum count, as shown in the color bar. Three representative areas are marked using white boxes (ROI1, ROI2, and ROI3). b Hα light curve in ROI 1. The vertical lines indicates five time points before, during, and after the flare. The corresponding NIR intensity profiles (Stokes I) are plotted in (c), from which we see almost identical line profiles indicating that the flare heating almost has no effect in this deep layer of solar atmosphere. d Hα light curve in ROI 2. The corresponding NIR intensity profiles at t0, t1, and t2, are plotted in (f). e Hα light curve in ROI 3. The corresponding NIR intensity profiles at t0-t4 are plotted in (g)
