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k(p) = k„(p)cos2 Y + K±(p)sin2 Y; k„(p) = -vl; kl(j>) = vvp±, (3.12.27)

where mH = ZeH-F(p); v(p) = no)HmRW(or)/4Pm; mR = {yAjv)ct)H . (3.12.28)

Approximately orW(or) = 2Pw, and for ~2 GeV (v ~ c ), ro = 60 AU we find the expected dependence of krr(Ek) on r (see Fig. 3.12.3).

Fig. 3.12.3. Expected CR radial diffusion coefficient Krr (Ek) for CR particles with kinetic

energy 2 GeV in units 10 cm /sec as function of heliocentric distance r. According to Zirakashvili et al. (1991).

Fig. 3.12.3. Expected CR radial diffusion coefficient Krr (Ek) for CR particles with kinetic

energy 2 GeV in units 10 cm /sec as function of heliocentric distance r. According to Zirakashvili et al. (1991).

In Fig 3.12.4 is shown the expected dependence of PcjpouO and ufuo from r at r > ro = 60 AU

Fig. 3.12.4. Ratio of CR pressure to initial dynamic pressure of the solar wind and ratio of the solar wind speed u to initial speed uo = 400 km/s as functions of distance r. According to Zirakashvili et al. (1991).

It follows from Eq. 3.12.22 that the terminal transition will be of shock wave type only in the case when

Pou0

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