E1E2e TiO0 G1520 Pc PC1sPC20 31118

uo uo Po and it is assumed that

Then the Eq. 3.11.14 takes the form

os Po ds po os and the Eq. 3.11.15, considering the condition described by Eq. 3.11.19, will be transformed into

After separating the variables with due account of the condition described by Eq. 3.11.19, the continuity Eq. 3.11.16 will be

T1 ds Pc2sine d0

Here K1 in Eq. 3.11.21 and K2 in Eq. 3.11.22 are separation constants. Thus, knowing the angular dependence of galactic CR pressure (for example, on the basis of the solution for the anisotropic diffusion equation) we may find the angular dependence of the 0 -component of the velocity of inhomogeneous solar wind.

It will be noted that we may obtain for Pc2 by combining the Eq. 3.11.21 and Eq. 3.11.22 the following equation:

I' \ ~\2 p p cos2 e -1) d c2 + 2cos e-rPc^-) + KK2Pc2 = 0 (3.11.23)

the solution for which is the Legendre polynomials of the order of n at K1K2 =

-n(n+1). The Eq. 3.11.20-3.11.23 may be used to obtain the differential equation for determining the radial dependence of the angular component of the solar wind velocity determaining the meridional motion d_ ds f 2 uoK2T1

dG ds

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