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We employ coronal extrapolations of solar magnetograph data to interpret observations of the whitelight streamer structure made with the LASCO coronagraph in 1996. The topological appearance of the streamer belt during the present minimum activity phase is well described by a model in which the Thomson-scattering electrons are concentrated around a single, warped current sheet encircling the Sun. Projection e ects give rise to bright, jet-like structures or spikes whenever the current sheet is viewed edge-on ; multiple spikes are seen if the current sheet is sufficiently wavy. The extreme narrowness of these features in polarized images indicates that the scattering layer is at most a few degrees wide. We model the evolution of the streamer belt from 1996 April to 1996 September and show that the e ect of photospheric activity on the streamer belt topology depends not just on the strength of the erupted magnetic ux, but also on its longitudinal phase relative to the background eld. Using ux transport simulations, we also demonstrate how the streamer belt would evolve during a prolonged absence of activity.
Wang et al. (Wed,) studied this question.