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By Nicole Meyer-Vernet

Advent to sunlight wind for researchers and graduate scholars in atmospheric physics and astrophysics.

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Basics of the Solar Wind

Creation to sun wind for researchers and graduate scholars in atmospheric physics and astrophysics.

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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.

5 1. [10] Eather, R. H. 1980, Majestic Lights, Washington DC, American Geophysical Union. [11] Egeland, A. and W. J. Burke 2005, Kristian Birkeland: The First Space Scientist, New York, Springer. [12] Fitzgerald, G. F. 1892, Sunspots and magnetic storms, The Electrician 30 48. [13] Foukal, P. V. 2004, Solar Astrophysics, New York, Wiley. G. 1984, Secrets of the Sun, Cambridge University Press. [15] Haigh, J. D. et al. eds. 2004, The Sun, Solar Analogs and the Climate, New York, Springer. [16] Harten, R.

Trans. Roy. Soc. London A 358 657. [30] Vsekhsvjatsky, S. K. 1963, in The Solar Corona, ed. J. W. Evans, London, Academic Press, p. 271. -P. 1980, The scientific objectives of the international solar polar mission, Phil. Trans. Roy. Soc. London A 297 565. -P. 1992, The Ulysses mission, Astron. Astrophys. Suppl. Ser. 92 207. [33] Zirker, J. B. 2002, Journey from the Center of the Sun, Princeton University Press. 2 Tool kit for space plasma physics Most of the Universe is made of plasma. And yet, plasmas are very rare on the Earth, where solids, liquids and gases – the three primary states of matter – are ubiquitous (Fig.

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