Jr KrrT77 udrrn J O Kdr T77

rsinOd< dr r dO rsinOd<

Let us now determine the flux JR = ndR/dt relative to the rigidity axis caused, by the fact that in the case of radial divergence of magnetic inhomogeneities from the Sun, there is a systematic loss of particle energy owing to prevailing scattering at the overtaking collisions (in the directions d and p) (Ginzburg et al., 1955).

Since the particle energy E is decreased in average by AE = - EvAu/c2 in an elementary collision act ( Au = uA/r ), the time between two collision is At = A/v, and the energy decrease takes place only for the directions normal to r (in the directions d and p ), we shall have dE dt


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