and the subscript 1 denotes that these values are taken at r = r\ = 1 AU.
In the work Babayan and Dorman (1979) it was assumed, according to the results of Fite et al. (1962), that a cross-section for the process of re-charging protons of solar wind is independent of energy and equal to
As to the density N^o of interstellar neutral hydrogen in a vicinity of the solar system, there is still a great uncertainty: in various works, the values of NHo from 10 to 0.05 cm-3 are presented (Baranov and Kransnobaev, M1977; Holzer, 1972). Therefore, the calculations were made for the values N^o = 0.1, 0.5 and 1 cm-3. The interstellar spectrum of galactic CR was taken as well as above in Section 3.7.2, in the form of a power spectrum on kinetic energy and rigidity of particles, and the transport path A for scattering of particles in interplanetary space was taken which respect to Eq. 3.7.8 at ft = 0, 0.5 and 1. Fig. 3.7.7 shows, as an example, the expected variation of solar wind velocity with a distance from the Sun r for N^o =
0.1, 0.5 and 1 cm- , ft = 0, solar wind velocity u = 3x10 cm/sec and its density N1 = 5 cm-3 near the Earth's orbit.
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