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Fig. 3.7.6. Modulation depth n/no at various distances from the Sun r/rj including non-

linear interaction of CR with solar wind at uj = 3 xl0 cm/sec, Nj = 5 cm , 3 = 0,

no ^ Ek ■ , Ek min = 0.01 GeV. Curves 1 —5 are respective to particles with the rigidities 0.5, 1.0, 5.0, 10, and 100 GV.

3.7.3. Radial braking of solar wind and CR modulation: effects of galactic CR pressure and re-exchange processes with interstellar neutral hydrogen atoms

The importance of including the effect of the re-charging of neutral hydrogen for a deceleration of solar wind was emphasized by Parker (M1963). A relative contribution of this effect depends on a number of factors and, first of all, on the density of neutral hydrogen in the vicinity of the solar system. The effect under consideration was taken into account in the papers Axford and Newman (1965), Sousk and Lenchek (1969), Semar (1970), etc. The complete equation set determining a propagation of solar wind in a spherically symmetric model, including a modulation of galactic CR and the phenomenon of re-charging of neutral hydrogen was obtained and solved by means of computer in the work Babayan and Dorman (1979).

The set of hydrodynamical equations that determines the solar wind propagation, taking into account the CR pressure Pc and re-exchange between solar wind protons and atoms of interstellar neutral hydrogen is given below:

Fig. 3.7.6. Modulation depth n/no at various distances from the Sun r/rj including non-

linear interaction of CR with solar wind at uj = 3 xl0 cm/sec, Nj = 5 cm , 3 = 0,

no ^ Ek ■ , Ek min = 0.01 GeV. Curves 1 —5 are respective to particles with the rigidities 0.5, 1.0, 5.0, 10, and 100 GV.

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