In this case, A// « p2- v . The contribution of strong random scattering is significant at any strengths of the random magnetic field. The momentum dependence of A // in this case is similar to that numerically calculated by Teufel and Schlickeiser (2002, 2003) and Shalchi and Schlickeiser (2004).
For protons with energy of 200 MeV scattered in a weakly disturbed interplanetary medium, substituting R = 4 x1010 cm, L// = L± = 2 x1012 cm, v = 1.67,
and Q ¡m = 8 yields A// = 0.25 AU. This value of A// is close to the mean experimental values from Palmer (1982). The values of A // are close to those from Shalchi and Schlickeiser (2004), in which, however, slab turbulence produces the main scattering. Thus, the weak momentum dependence of A // for solar CR over a wide energy range from several MeV to several GeV can be explained in terms of strong (moderate) random scattering by two-dimensional turbulence in the solar wind.
In the case of the very strong turbulence in co-rotating interaction region of the outer Heliosphere
Was this article helpful?