By Nicole Meyer-Vernet
Creation to sunlight wind for researchers and graduate scholars in atmospheric physics and astrophysics.
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Additional resources for Basics of the Solar Wind
1959, Round-table discussion, J. Geophys. Res. 64 1691.  Title, A. 2000, Magnetic ﬁelds below, on and above the solar surface, Phil. Trans. Roy. Soc. London A 358 657.  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.  Zirker, J. B. 2002, Journey from the Center of the Sun, Princeton University Press.
1). These states are the result of a competition between thermal energy and intermolecular forces. In solids, the latter win, maintaining the atoms and/or molecules at nearly ﬁxed positions, whereas thermal energy merely produces vibrations around these positions . In gases on the contrary, thermal energy wins, making the particles almost completely free. Liquids are in between: the intermolecular forces are suﬃciently strong to resist compression, but suﬃciently weak to enable deformation and ﬂow; it is not surprising that this intermediate state is less well understood than the other two .
More may be found in several excellent texts, for example , , , , ,  and . 1 What is a plasma? In any gas there are always a few atoms or molecules that manage to lose one electron, producing some small degree of ionisation. Being ionised is therefore What is a plasma? 43 not suﬃcient to qualify as a plasma. A useful deﬁnition may be instead that a plasma is: • a gas1 containing charged particles (together with neutral ones), which • is quasi-neutral • and exhibits collective behaviour.
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