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It is obvious that a focusing action of CR onto solar wind will be substantial if x^(r) is comparable to r6o. The numerical calculations were made by Babayan and Dorman (1977b) with respect to Eq. 3.11.8 and Eq. 3.11.9 including Eq. 3.7.8, Eq. 3.7.9, and Eq. 3.7.11 for CR interstellar spectrum of the form described by Eq. 3.7.7 for the values of y = 1.5 and 2.0; Ek ,min = 0.1 and 0.01 GeV. The values of A were taken as the same as in Section 3.7. The velocity and density of solar wind on the Earth's orbit were set to be U1 = 3 x107 and 4 x107 cm/sec, A1 = 5 and 10 cm-3. In Fig. 3.11.1 the expected values of u^(r) and x±_(r)/r0o are presented at y = 1.5,

U1 = 3 x107 cm/sec and A1 = 5 cm-3. It is seen that u±(r) is initially increased, then it starts to diminish with distance. It is connected with Pc(r) tending to Pco at great distances. The calculations were made up to the distances where the radial velocity of solar wind falls by an order compared to its initial value, owing to non-linear interaction with CR in the radial direction, with respect to the results of Sect. 3.7.

Fig. 3.11.1. Expected u1(r) and x±(r)/rQo (a and b, respectively), for y = 1.5; u1 = 3x107 cm/sec, N1 = 5cm-3 . Curve 1 for Ekmi„ = 0.1 GeV, do = 30°; 2 - for Ekmi„ = 0.1 GeV. do = 25°; 3 - for Ekmin = 0.01 GeV, do = 30°, 4 - for Ekmin = 0.01 GeV, do = 25°.

Fig. 3.11.1. Expected u1(r) and x±(r)/rQo (a and b, respectively), for y = 1.5; u1 = 3x107 cm/sec, N1 = 5cm-3 . Curve 1 for Ekmi„ = 0.1 GeV, do = 30°; 2 - for Ekmi„ = 0.1 GeV. do = 25°; 3 - for Ekmin = 0.01 GeV, do = 30°, 4 - for Ekmin = 0.01 GeV, do = 25°.

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