k min

Nonlinear Cosmic Ray Effects in Space Plasmas Fig. 3.7.2 presents the same as Fig. 3.7.1 but for ß= 1.

Nonlinear Cosmic Ray Effects in Space Plasmas Fig. 3.7.2 presents the same as Fig. 3.7.1 but for ß= 1.

0 50 100 150 200 250 300 350 400 17 f,

Fig. 3.7.2. The same , as in Fig. 3.7.1, but at 0= 1.

0 50 100 150 200 250 300 350 400 17 f,

Fig. 3.7.2. The same , as in Fig. 3.7.1, but at 0= 1.

A comparison of Fig. 3.7.1 and Fig. 3.7.2 shows that a variation of solar wind velocity is strongly dependent on how A depends on r//j . In the first case the velocity falls by an order at the distances 85, 32, 9 AU, whereas in the second case this occurs at the distances 140 and 22 AU for Ek ,min = 0.01 and 0.001 GeV, and at

Ek ,min = 0.1 GeV even at the distance 400 AU, the velocity falls down only by 3 times.

Fig. 3.7.3 presents the results of calculations for spectrum described by Eq. 3.7.7 with y = 2 and 0 = 0. It easy to see that in this case a braking takes place at substantially less distances than with y = 1.5. In particular, curve 3 shows that the wind velocity falls down by ten times yet at the distances ~ 5 AU at Ek ,min = 0.001 GeV. This is connected with that a density of kinetic energy of CR in this case is of

Fig. 3.7.3. Dependence of UU1 on r/r for the case U1 = 3 x 107 cm/sec, N1 = 5 cm-3 , 0 = 0, y = 2, no E-3 0. Curve 1 for Ekmin = 0.1 GeV; 2 - for Ekmin = 0.01 GeV, 3 - for Ek min = 0.001 GeV.

In Fig.3.7.4 the same is shown as in Fig. 3.7.1 but at u = 4x 10 cm/sec and N1 = 10 cm-3. In this case the wind's deceleration is substantially weaker than for the variants shown in Fig. 3.7.1. This means that a deceleration of the solar wind is essentially dependent on the parameter characterizing the solar activity (a velocity of the wind and its density near the Earth's orbit).

Fig. 3.7.4. Dependence of u/u1 on r/r for the case u = 4 x 107 cm/sec, N = 10 cm-3, ft

= 0, no rc E-2'5. Curve 1 for Ekmin = 0.1 GeV; 2 - for Ekmin = 0.01 GeV, 3 - for

Fig. 3.7.4. Dependence of u/u1 on r/r for the case u = 4 x 107 cm/sec, N = 10 cm-3, ft

= 0, no rc E-2'5. Curve 1 for Ekmin = 0.1 GeV; 2 - for Ekmin = 0.01 GeV, 3 - for

The results of calculations for the rigidity spectrum are presented in Fig. 3.7.5. The dependence on Rmin is weaker that for spectra over Ek . It is connected with that in the case of rigidity spectrum, Wqr is weakly dependent on Rmin .

Fig. 3.7.5. Dependence of u/u on r/r for the case u = 3x10 cm/sec, N = 5cm , ¡3=

0, no rc R"2-5. Curve 1 for Rmin = 0.1 GV; 2 - for Rmin = 0.01 GV, 3 - for Rmin = 0.001 GV.

nONLINEAR cOSMIC rAY eFFECTS IN sPACE pLASMAS

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