The energy spectrum of primary cosmic rays above 10¹²eV

Turbulent diffusion and drift in galactic magnetic fields and the explanation of the knee in the cosmic ray spectrum

“…Figure 5 shows the results for a source localized at r s = 3 kpc with the same random field as in Figure 2, for the NR − S case and for both signs of B d · B h , as indicated. The possible existence of a feature similar to this one in the actual data was first noticed by Kempa et al [26] many years ago but still remains somewhat controversial. It is however interesting to notice that the present scenario naturally provides a variety of results with the ability of reproducing diverse observations.…”

Liquid phase epitaxial growth of GaInAsP/InP laser structures

“…The pronounced bump observed in figure 2 for this case is in disagreement with the observed spectra, so that this model would be observationally disfavored. However, the possible existence of a smaller bump just below the knee in the actual data was noticed by Kempa et al [26] many years ago, although it still remains somewhat controversial. It is interesting however that features of this kind may arise from drift effects in some particular configurations of regular galactic magnetic fields.…”

Fine structure in the cosmic ray spectrum: Further analysis and the next step

“…Turning to curvature in the energy spectrum just before the knee, its presence in the total particle spectrum has been known for a long time (see, for example, Kempa et al, 1974) and it is due to the imminent appearance of the peak due to the single source. There is evidence that the curvature is finite at lower energies too, and occurs at similar rigidity for all nuclei.…”