Cosmic-ray-driven galactic wind

Anisotropic diffusion of Galactic cosmic ray protons and their steady-state azimuthal distribution

“…The spatial diffusion, in general, should be described by a tensor, but in most applications to Galactic propagation so far, it is simplified to a scalar coefficient κ s , i.e.κ = (κ i j ) = (δ i j κ s ) (see the discussion above). An ordered motion of the ISM can be taken into account via the convection velocity u (e.g., Fichtner et al 1991;Ptuskin et al 1997;Völk 2007), but is neglected for this study due to its decreasing importance for higher CR energies. Continuous momentum losses are described by the momentum change ratė p. Catastrophic loss processes, such as spallation, do not apply, since in this study only Galactic protons are considered.…”

“…κ = (κ i j ) = (δ i j κ s ) (see the discussion above). An ordered motion of the ISM can be taken into account via the convection velocity u (e.g., Fichtner et al 1991;Ptuskin et al 1997;Völk 2007), but is neglected for this study due to its decreasing importance for higher CR energies. Continuous momentum losses are described by the momentum change rate ṗ.…”