Confinement and anisotropy of ultrahigh-energy cosmic rays in isotropic plasma wave turbulence. I. Modification of the Hillas limit due to turbulence geometry

Details Confinement and anisotropy of ultrahigh-energy cosmic rays in isotropic plasma wave turbulence. I. Modification of the Hillas limit due to turbulence geometry Confinement and anisotropy of ultrahigh-energy cosmic rays in isotropic plasma wave turbulence. I. Modification of the Hillas limit due to turbulence geometry

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...467...15v&link_type=abstract

Astronomy and Astrophysics, Volume 467, Issue 1, May III 2007, pp.15-20

Astronomy and Astrophysics

Astrophysics

2

Ism: Cosmic Rays, Ism: Magnetic Fields, Plasmas, Scattering

Scientific paper

Context: The mean free path and anisotropy of galactic cosmic rays is calculated in weak plasma wave turbulence that is isotropically distributed with respect to the ordered uniform magnetic field. Aims: The modifications on the value of the Hillas energy, above which cosmic rays are not confined to the Galaxy, are calculated. The original determination of the Hillas limit has been based on the case of slab turbulence where only parallel propagating plasma waves are allowed. Methods: We use quasilinear cosmic ray Fokker-Planck coefficients to calculate the mean free path and the anisotropy in isotropic plasma wave turbulence. Results: In isotropic plasma wave turbulence the Hillas limit is enhanced by about four orders of magnitude to E_c=2.03 × 10^5An_e1/2(L_max/10~pc) PeV resulting from the dominating influence of transit-time damping interactions of cosmic rays with obliquely propagating magnetosonic waves. Conclusions: Below the energy Ec the cosmic ray mean free path and the anisotropy exhibit the well known E1/3 energy dependence. At energies higher than Ec both transport parameters steepen to a E^3-dependence. This implies that cosmic rays even with ultrahigh energies of several hundreds of EeV can be rapidly pitch-angle scattered by interstellar plasma turbulence, and are thus confined to the Galaxy.
Appendices are only available in electronic form at http://www.aanda.org

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