By L. Marton (Ed.)
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T Obviously, for this purpose the solar wind must be described by kinetic theory rather than fluid theory. 18 AARON BARNES determined by the interplanetary magnetic and electrostatic fields (Eviatar and Schulz, 1970; Schulz and Eviatar, 1972; Perkins, 1973). If it is assumed that the electron flow is noncollisional beyond some point, a number of plasma instabilities may arise (Schulz and Eviatar, 1972). Schulz and Eviatar have outlined some of the effects that such instabilities may have on the transport properties of the solar wind.
This relatively simple model is based on the assumptions of radial, steady, spherically symmetric flow, that the acceleration is governed by fluid pressure and gravity, and that the heating is due to thermal conduction. The transport coefficients are taken to be due to Coulomb collisions, but viscosity is neglected. Then the flow is described by the equation of continuity, nu? , the momentum equation, nm,u(du/dr) + (d/dr)[nk(T,+ T,)] + (GM,m,n/r2) = 0, (28) 30 AARON BARNES and the electron and proton heat equations, The expressions for the electron and proton thermal conductivities, K , and K , , and the energy-exchange rate vE are those given by Braginskii (1965).
The density, temperatures, and magnetic field are held fixed at the base of all models of the series. For definiteness, the wave spectrum was taken to be monochromatic, but the results are not sensitive to this assumption or to the choice of frequency. , 1969). These models also included the usual assumptions of spherically symmetric, steady flow. The dynamical equations of the flow are Eqs. (27)-(30), with the exception that the heating of ions due to Landau damping of the waves is added to Eq.
Advances in Electronics and Electron Physics, Vol. 36 by L. Marton (Ed.)