Abstract
We analyze calibrated white-light coronal images from the LASCO-C2/SOHO experiment (processing level L1), focusing on quasistationary events without coronal mass ejections or their manifestations in the solar wind. The previous result that the streamer belt forms a set of rays of increased brightness is confirmed. The cross section of the streamer belt is frequently observed as two closely spaced rays differing in brightness. It is difficult to explain this in terms of ordinary bending of the belt. We suggest that the belt is normally a set of pairs of rays with enhanced brightness (or two close rows of rays). The distance between the rays in each pair is comparable to the ray size. The ray brightnesses in any pair can, in general, be different. The magnetic field has opposite directions in the rays forming a pair, so that the neutral line of the radial component of the solar magnetic field probably runs along the strip between the pairs of rays.
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