By Nicole Meyer-Vernet
Creation to sunlight wind for researchers and graduate scholars in atmospheric physics and astrophysics.
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Additional info for Basics of the Solar Wind
22). The coronal image on which the data are superimposed shows the simple structure we have already seen in the left-hand panel of Fig. 12, with dark coronal holes on the polar caps and bright streamers extending outwards near the equatorial plane. The solar wind structure reﬂects this simplicity: the speed is nearly constant at all latitudes except in a narrow band of ±20◦ around the equator where the speed pattern resembles the two-state structure seen by near-ecliptic spacecraft. This simplicity is shared by the other properties.
On this ﬁgure, the speed is plotted in 20 The speed is from the SWOOPS particle electrostatic analyser (Bame, S. J. et al. 1992, Astron. Astrophys. Suppl. Ser. 92 237), and the density from thermal noise analysis of data from the URAP instrument (Stone, R. G. et al. 1992, Astron. Astrophys. Suppl. Ser. 92 291), that are the best ways of measuring these respective properties on Ulysses (Issautier, K. et al. 1999, J. Geophys. Res. 104 6691). 22 Solar wind speed as a function of heliocentric latitude, plotted in polar co-ordinates during Ulysses’ ﬁrst two orbits.
6) the so-called Debye length.