The amplitude of magnetohydrodynamic turbulence in the inner solar wind

Recent radio wave interplanetary scintillation observations have improved our knowledge of the level of turbulent fluctuations of plasma density in the inner solar wind at heliocentric distances of 16-26 R-. and less accurately outside this range. This information relates to fluctuations in the inertial subrange of the turbulence. Of particular concern in this paper is the heliocentric distance dependence of the power-law normalization parameter C-N(2). This measurement of C-N(2), when combined with independent measurements of the mean plasma density in the inner solar wind, indicates that the dimensionless amplitude of the turbulence epsilon = sigma(n)/(n) over bar is low, of the order of 6%-15%, where sigma(n) is the standard deviation of the density fluctuations and (n) over bar is the mean value. The deduced value for epsilon depends on an assumed value for the outer scale of the turbulence, l(o). I adopt a fiducial value of l(o) = 1 R-.. A comparison is made with independent estimates of epsilon, from both radio remote sensing in the same part of space and in situ measurements at greater distances. Satisfactory agreement occurs. I discuss the possibility that this dimensionless density amplitude epsilon might be a proxy for the corresponding amplitude of the magnetic field fluctuations. This is a controversial assertion. However, if it is the case, the measurements suggest that the turbulence in the inner solar wind is weak, in the sense of being dynamically and thermodynamically important.