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

Figure 1

(a) Maximum percentage difference between 𝐁_Pol and 𝐁_Par as a function of the solar distance inside the colatitude regions 20^∘≤𝜃≤160^∘ (𝜃₂₀^∘), 25^∘≤𝜃≤155^∘ (𝜃₂₅^∘), and 30^∘≤𝜃≤150^∘ (𝜃₃₀^∘). (b) Maximum value allowed of 𝛿_𝑚 as a function of colatitude: values in the “allowed” region guarantee that the stream line originated from the polar magnetic field do not cross the equatorial plane. Since (5) is symmetric with respect to the solar equatorial plane, values greater than 90^∘ of colatitude lead to same results of those presented.

(a)

(b)