The solar sources of slow solar wind

Details The solar sources of slow solar wind The solar sources of slow solar wind

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..223b&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 223-226 (1999).

Computer Science

Particle Emission, Solar Wind, Interplanetary Magnetic Fields

Scientific paper

During its solar wind scanning from pole to pole, Ulysses observed an equatorial band of slow solar wind of +/-20°, corresponding to regions above the equatorial coronal helmets. Recently it has been argued that the slow solar wind comes from narrow bright regions called ``stalks,'' that are the extension of coronal helmets. In this paper we use Hoeksema's potential field model of the structure of the solar magnetosphere for the times of Ulysses' solar poles flyby and for the time of the observation of a stalk to determine the magnetic characteristics of such sources. We find that the slow wind observed by Ulysses at low latitude originated from the bordering regions of both polar coronal holes, which bend toward the equator, and from small, low-latitude holes. The comparison of magnetic field structures and plasma density structures shows that stalks are the convergence region of the open magnetic field lines of different polarity, which are bordering helmets.

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