Summary of Chapters 1 2 and

It may be useful to summarize in a few paragraphs what I have learned from the IGY period to the end of the 1980s and what I described in Chapters 1, 2, and 3. The solar wind and the magnetosphere constitute a dynamo (Figure 4.28). Its power is represented by e VB2 sin4 (0 2) 2 (see Section 1.9). When the power exceeds 1018 erg sec or so, the magnetosphere becomes primed as the north and south solenoidal currents in the magnetotail, including the cross-tail current, are intensified. During this...

Flux Ropes Observed in Interplanetary Space

Burlaga et al. (1981), Burlaga and Klein (1982), Marubashi (1986), Burlaga (1988, 1995), and many others have shown that some passing magnetic structures in the disturbed solar wind can be approximated by a cylindrical force-free field (J x B 0), Figure 8.11. The helical structure they found can most easily be identified by characteristic changes of the north-south component of the IMF, when B, Bx, By, and Bz (or theta) are plotted as a function of time (Figure 8.12). During the passage of such...