By Nicole Meyer-Vernet
Advent to sun wind for researchers and graduate scholars in atmospheric physics and astrophysics.
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Книга откроет вам все возможные секреты, как уложить малыша спать без слез
Extra resources for Basics of the Solar Wind
Near activity maximum, therefore, the pattern of alternating fast and slow streams is observed at all latitudes, with, however, somewhat smaller speeds and scales than near activity minimum. 3 A simpliﬁed three-dimensional picture These Ulysses observations bear out – albeit with some modiﬁcations – a simple picture of the heliosphere near solar activity minimum, that had already been 21 The values of ρv and ρv 2 are slightly greater than nm v and nm v 2 respectively because p p there is a small proportion of helium.
A. et al. 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.
26. As the Sun spins, the WIND spacecraft in the ecliptic lies alternately above and below the heliospheric current sheet. At each crossing of the sheet, the direction of the magnetic ﬁeld changes and a slow and variable wind is observed. This picture is also consistent with observations from Ulysses, which spends most of its trajectory far from the current sheet near solar minimum, and measures a fast stationary wind with a constant magnetic polarity in each solar hemisphere except at low latitudes.
Basics of the Solar Wind by Nicole Meyer-Vernet