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1.M. Neugebauer and C. W. Snyder, J. Geophys. Res. 71, 4469 (1966).
2.M. Neugebauer and C. W. Snyder, J. Geophys. Res. 72, 1823 (1967).
3.L. Davis, Jr., E. J. Smith, P. J. Coleman, Jr., and C. P. Sonett, The Solar Wind (Pergamon Press, Inc., New York, 1966), p. 35.
4.P. J. Coleman, Jr., Phys. Rev. Letters , 17, 207 (1966).
5.P. J. Coleman, Jr., Planet Space Sci. 15, 953 (1967).
6.A. Barnes, Phys. Fluids 9, 1483 (1966).
7.P. J. Coleman, Jr., Ph.D. thesis, University of California at Los Angeles (1966).
8.E. H. Holt, and R. E. Haskell, Foundations of Plasma Dynamics (Macmillan Company, Inc., New York, 1965), Chap. 14.
9.W. B. Thompson, An Introduction to Plasma Physics (Pergamon Press, Inc., New York, 1962), Chap. 5.
10.Uncertainties in these data arise from the digitization of the output voltages before telemetering. For the magnetometer, the digitization uncertainty is which, though small compared to the uncertainty in the determination of the spacecraft field and the magnetometer zero offsets, is the important uncertainty when considering short period variations in the field. The resulting uncertainties in the value of υ calculated from the magnetic field variations are indicated in Figs. (6), (7), and (8), together with the digitization uncertainties in the measured υ divided by For each density measurement, the digitization uncertainty is ±13%.
11.The Alfvén velocity is a function of density; hence, a second iteration of the computer solutions was necessary.

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