Papers › The theory of cosmic-ray scattering on pre-existing MHD modes meets data
The theory of cosmic-ray scattering on pre-existing MHD modes meets data
Ottavio Fornieri, Daniele Gaggero, Silvio Sergio Cerri, Pedro De la Torre Luque, Stefano Gabici
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We present a comprehensive study about the phenomenological implications of the theory describing Galactic cosmic-ray scattering onto magnetosonic and Alfv\'enic fluctuations in the GeV - PeV domain. We compute a set of diffusion coefficients from first principles, for different values of the Alfv\'enic Mach number and other relevant parameters associated to both the Galactic halo and the extended disk, taking into account the different damping mechanisms of turbulent fluctuations acting in these environments. We confirm that the scattering rate associated to Alfv\'enic turbulence is highly suppressed if the anisotropy of the cascade is taken into account. On the other hand, we highlight that magnetosonic modes play a dominant role in Galactic confinement of cosmic rays up to PeV energies. We implement the diffusion coefficients in the numerical framework of the {\tt DRAGON} code, and simulate the equilibrium spectrum of different primary and secondary cosmic-ray species. We show that, for reasonable choices of the parameters under consideration, all primary and secondary fluxes at high energy (above a rigidity of ≃200 GV) are correctly reproduced within our framework, in both normalization and slope.
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