ZeVAp3fe p r

For r = ro = 60 AU, v = c, 9 = n/2 we obtain A ~ 20%. The expected dependence of Krr from kinetic energy of particles is shown in Fig. 3.12.1, the expected depth of modulation in the outer Heliosphere fo/fe in the interval 40-60 AU is in Fig. 3.12.2.

Fig. 3.12.1. CR radial diffusion coefficient Krr E ) in units 1021 cm2/sec at heliocentric distances 40 AU (assumed according to spaceprobe measurements) and as expected at 60 AU (as developed from CR kinetic stream instability calculated in Dorman et al., 1990).

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