By L. Marton (Ed.)
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Extra resources for Advances in Electronics and Electron Physics, Vol. 36
The wave tends to pick up resonant particles of mass m and magnetic moment p = fmv:/B because of its gradient in magnetic field strength, - m d v l l / d t = -P(VB),~. ) The process by which this resonant acceleration leads to exchange of energy between waves and particles has been analyzed in detail by Barnes (1967). For an isotropic velocity distribution the energy exchange is proportional to the derivative d f l d u , , of the velocity distribution evaluated at u I I = co/k,,; this energy exchange may involve either electrons or ions.
The agreement between theory and observation is excellent for u I 425-450 km sec-', which corresponds to most of the observations. Theory and observation do not agree well at higher velocities. However, dispersion in the scatter plot suggests that the Tp-u correlation is not strong at the higher velocities; this may indicate that nonsteady effects strongly influence the temperature in high velocity streams. , 1971) gives another comparison of the series of models with the observed Tp-u correlation.
Iv. ACCELERATION A N D HEATING OF THE SOLAR WIND A . Introductory Remarks The question of heating has been fundamental to theoretical studies of the solar wind ever since Parker’s original prediction. At such temperatures hydrogen is fully ionized and has very high thermal conductivity. 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.
Advances in Electronics and Electron Physics, Vol. 36 by L. Marton (Ed.)