By Nicole Meyer-Vernet
Advent to sunlight wind for researchers and graduate scholars in atmospheric physics and astrophysics.
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Additional info for Basics of the Solar Wind
F. 1892, Sunspots and magnetic storms, The Electrician 30 48.  Foukal, P. V. 2004, Solar Astrophysics, New York, Wiley. G. 1984, Secrets of the Sun, Cambridge University Press.  Haigh, J. D. et al. eds. 2004, The Sun, Solar Analogs and the Climate, New York, Springer.  Harten, R. and K. Clark 1995, The design features of the GGS Wind and Polar spacecraft, Space Sci. Rev. 71 23.  Kippenhahn, R. 1994, Discovering the Secrets of the Sun, New York, Wiley.  Lemaire, J. and V. Pierrard 2001, Kinetic models of solar and polar winds, Astrophys.
Furthermore this plasma manages to ﬂow outwards, with an energy density greater than that of the magnetic ﬁeld, as we will see in Chapters 5 and 6. How does this modify the picture? 3) that the plasma and the magnetic ﬁeld lines are strongly tied together, so that the plasma can move along the ﬁeld lines but not across them, just as beads on a necklace. Near the poles, where the magnetic lines extend nearly radially, the outgoing wind can ﬂow unimpeded along them. In the equatorial regions, however, the situation is diﬀerent because an outgoing wind would have to ﬂow perpendicularly to the dipolar ﬁeld lines (Fig.
Having cooled, the material is denser and sinks back into the Sun. The upward ﬂow in the central region of the granules compensates for this disappearing cold material. Granulation is not the only structure presumably convective in origin observed at the photosphere. It is the most conspicuous of what may be a continuum of convective ﬂow scales. In particular, a large-scale velocity pattern – the so-called supergranulation – is observed, albeit with little if any intensity contrast. 5 km s−1 towards the periphery of the cells, with much slower vertical upﬂows at the centre of the structures and downﬂows at their boundaries.
Basics of the Solar Wind by Nicole Meyer-Vernet