Latitudinal Dependence of Cosmic Rays Modulation at 1 AU and Interplanetary Magnetic Field Polar Correction

Table 6

Average values (last three columns) of 𝜂_rms (in percentage, %) as a function of 𝛿_𝑚 (×10⁻⁵) and 𝜌_𝑘, for BESS-1997, AMS-1998, PAMELA-2006/08, obtained from (17) without enhancement of the diffusion tensor along the polar direction (𝜌_𝐸=1), using “R” and “L” models for the tilt angle and No Drift approximation. The differential intensities were calculated accounting for particles inside the heliospheric regions for which solar latitudes are lower than |5.7^∘|.

𝛿𝑚(×10^−5)	𝜌𝑘	“R” model	“L” model	No drift
0.0	0.10	14.1	11.0	33.4
1.0	0.10	11.7	8.7	33.2
2.0	0.10	11.6	8.3	33.7
3.0	0.10	11.6	8.3	33.7
1.0	0.11	6.4	9.0	27.7
2.0	0.11	7.8	9.0	28.3
3.0	0.11	7.5	8.8	29.2
1.0	0.12	6.3	7.1	23.5
2.0	0.12	6.3	7.3	24.7
3.0	0.12	7.1	6.9	24.4
1.0	0.13	6.3	6.4	20.1
2.0	0.13	6.6	7.6	20.4
3.0	0.13	6.7	7.7	20.5
1.0	0.14	7.3	7.0	15.9
2.0	0.14	7.3	7.2	16.4
3.0	0.14	7.2	6.5	16.8