http://arxiv.org/abs/1503.04477
The interplanetary magnetic field near has a characteristic “sector” structure that reflects its polarity relative to the solar direction. Typically we observe large-scale coherence in these directions, with two or four “away” or “towards” sectors per solar rotation, from any platform in deep space and near the ecliptic plane. In a simple picture, this morphology simply reflects the idea that the sources of the interplanetary field lie mainly in or near the Sun, and that the solar-wind flow enforces a radial component in this field. Although defined strictly via the interplanetary field near one AU, recent evidence confirms that this pattern also appears clearly at the level of the photosphere, with signatures including not only the large-scale structures (e.g., the streamers) but also highly concentrated fields such as those found in sunspots and even solar flares. This association with small-scale fields strengthens at the Hale sector boundary, defining the Hale boundary as the one for which the polarity switch matches that of the leading-to-following polarity alternation in the sunspots of a given hemisphere.
H. Hudson, L. Svalgaard and I. Hannah
Tue, 17 Mar 15
32/79
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