Basics of the Solar Wind by Nicole Meyer-Vernet

By Nicole Meyer-Vernet

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

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15). Strangely enough, they have found that there is not a single wind but several – albeit one is more basic than the others. 1 Observing near the ecliptic Some subtleties of space exploration Most space probes lie close to the ecliptic – the plane in which the Earth and most of the planets orbit the Sun. There is a simple reason for that. A spacecraft leaving the Earth starts with a velocity vector equal to the Earth’s orbital velocity plus that provided by the launcher; since the Earth’s velocity is about 30 km s−1 and lies in the ecliptic plane, one must give to the spacecraft a velocity perpendicular to the ecliptic of at least this amount to put it into an orbit angled far from this plane; this is outside the capabilities of existing rocket technology (Fig.

24] Parker, E. N. 1997, in Cosmic Winds, ed. J. R. , Tucson AZ, University of Arizona Press, p. 3. [25] Parker, E. N. 2001, in The Century of Space Science, ed. J. A. M. , New York, Kluwer, p. 225. [26] Parker, E. N. 2001, A critical review of sun–space physics, Astrophys. Space Sci. 277 1. References 39 [27] Pneuman, G. W. and R. A. Kopp 1971, Gas–magnetic field interactions in the solar corona, Solar Phys. 18 258. [28] Simpson, J. A. et al. 1959, Round-table discussion, J. Geophys. Res. 64 1691.

They generally occur in groups on the solar disc. 8 (right panel) shows a detailed view of such a group,10 where individual spots appear as a dark umbra about 104 km across surrounded by a filamentary penumbra. Some sunspots may last for weeks; this has enabled early observers to follow their motion and to find that the Sun appears to rotate about its axis once in about 27 days (as seen from Earth). Detailed observation shows that the Sun does not rotate as a solid body: its outer layers rotate more slowly in polar regions than at the equator.

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