Astronomy and Astrophysics – Astronomy
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...553..198f&link_type=abstract
The Astrophysical Journal, Volume 553, Issue 1, pp. 198-210.
Astronomy and Astrophysics
Astronomy
15
Ism: Cosmic Rays, Ism: Magnetic Fields, Methods: Analytical, Plasmas
Scientific paper
We study the problem of cosmic-ray diffusion in the Galactic disk with particular attention paid to the problem of particle scattering through the θ=cos- 1(v∥/v)=90deg pitch angle in momentum space by wave-particle mirror interaction (here v∥ is the cosmic-ray velocity parallel to the average Galactic magnetic field). We consider the case in which cosmic rays are the only source of magnetic turbulence, which originates as the relativistic particles try to stream through the interstellar plasma faster than the local Alfvén speed. The wave growth rate is proportional to the cosmic-ray anisotropy, and the amplitude of hydromagnetic waves generated by this streaming instability is limited by the presence of various damping mechanisms. We study the propagation of cosmic rays in the different phases of the interstellar medium, in particular the coronal regions (where the main form of wave dissipation is nonlinear Landau damping) and the warm regions (where charge exchange between the ions and the neutral atoms gives rise to the dominant form of wave dissipation). We also account for ion-cyclotron damping of small wavelength waves. The effect of a spectrum of waves is to limit the anisotropy of the cosmic-ray distribution function and hence their drift velocity. We show that quasi-linear resonant scattering cannot account for particle diffusion everywhere in momentum space and that particles with θ~90deg must change their pitch angle by mirror interaction with long-wavelength waves generated by the θ~0deg particles. We match the quasi-linear scattering with the adiabatic mirroring in a small boundary layer in momentum space close to the θ~90deg point, and then we calculate the diffusion coefficient together with the cosmic-ray drift velocity. We show that scattering through the 90° point is very efficient, and we calculate the correction to the particle diffusion coefficient due to the presence of mirroring.
Felice G. M.
Kulsrud Russell M.
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