By L. Marton (Ed.)
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Additional resources for Advances in Electronics and Electron Physics, Vol. 36
In this model the state of the wind is determined by the wave energy efflux at the coronal base. The quiet state of the wind then corresponds to a relatively small, but nonzero, wave efflux. The three kinds of models described above may be compared with observations at 1 AU. , see Brandt, 1970; Newkirk, 1967) and the temperature near the coronal base. , 1972). All these models are in reasonable agreement with observation. In each case the agreement is not perfect, however. All these models suffer from a too flat density profile; the density is either too low near the sun or too high near 1 AU.
Finally, the Alfven waves of solar origin in the interplanetary medium strongly support the idea that the solar wind is turbulent throughout an envelope greater than 20 R , in radius. Altogether, this series of solar wind models, which is based on collisional thermal conduction with additional heating due to Landau damping of hydromagnetic waves, unifies a great variety of observations. It gives reasonable values of density, temperature, and flow speed at the orbit of the earth and near the sun.
On the other hand, the plasma density is so low ( 5 lo9 protons cmP3)that the corona is not an efficient radiator or absorber of light. Hence it is conceivable that the energy transport of the corona is largely governed by thermal conduction, which in turn means that the plasma temperature will decline slowly with heliocentric distance. In the idealized case in which the energy transport is entirely due to thermal conduction, and the magnetic field is radial, the temperature T is related to heliocentric distance Y by (Chapman, 1957) T ( r )= ~ ( u ) ( a / r ) ’ ’ ~ (4) LARGE-SCALE BEHAVIOR OF THE SOLAR WIND 19 (u is an arbitrary reference level).