-x-Adr=0.2 -Adr=0.3

- - Adr=0.4




Figure 2.46.11. The same as in Fig. 2.46.10, but for GOES data of protons with energy Ek > 100 MeV from January 1986 to December 1999. From Dorman et al. (2005c).

The best correlation is found again at ~ 0.1, but with maximum value 0.9793 at Xo max = 15 av. months, and regression equation ln(Icor) = -3.226 - 0.0525 x F , (2.46.24)

where F is determined by Eq. 2.46.9. From Eq. 2.46.24 it follows that the intensity out of Heliosphere lnIo =-3.226 (for GOES data of protons with energy Ek > 100 MeV). From the obtained results, according to Le Roux and Fichtner (1997) and Dorman et al. (2001b), we can estimate the dimension of modulation region

Cosmic Ray Propagation in Space Plasmas r0 = maxuef = 0.84X0maxu(i AU) 97.4 AU ,

and the effective radial diffusion coefficient

0.0525 av.month sec

2.46.7. The satellite alpha-particle data and their main properties

According to the procedure described in Sections 2.46.1-2.46.3 for the hysteresis analysis of small energy galactic CR fluxes, the following information is needed: kinetic energy interval, rigidity interval and effective rigidity Ref . These parameters are necessary for determining the coefficient Cav (Ref ), according to

Eq. 2.46.23, and diffusion time lag, T^f according to Eq. 2.46.22, for evaluating v/c interval and effective value (v/c )ef (for estimating the effective transport path of particles in the Heliosphere after the determination of diffusion coefficient). We used 5-minute GOES data of small energy alpha-particle fluxes (in units

—2 —i —i —i particles • cm • sec • sr • MeV ) from January 1986 to May 2000 in three energy intervals with parameters listed in Table 2.46.2 (

Table 2.46.2. Parameters for three used alpha-particles energy intervals.

Ek interval, MeV

R interval, GV

Ref, GV

Cav (Ref )

(v/c )ef



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