A semiempirical approach to low-energy cosmic ray propagation in the diffuse interstellar medium

Abstract

We investigate the ionization of the diffuse interstellar medium by cosmic rays by modeling their propagation along the wandering magnetic fields using a Monte Carlo method. We study how low-energy cosmic rays propagate in turbulent, translucent molecular clouds, and how they regulate the ionization and both lose and gain energy from the medium. As a test case, we use high spatial resolution (0.03 pc) CO maps of a well-studied high latitude translucent cloud, MBM 3, to model turbulence. The propagation problem is solved with a modified Monte Carlo procedure that includes trapping, energization, and ionization losses. In a homogeneous medium, trapping and re-energization do not produce a significant effect. In a nonuniform medium, particles can be trapped for a long time inside the cloud. This modifies the cosmic ray distribution due to stochastic acceleration at the highest energies (about 100 MeV). At lower energies, the re-energization is too weak to produce an appreciable effect. The change in the energy distribution does not significantly affect the ionization losses, so ionization changes are due to trapping effects.

8 pages, 13 figures

References in corpus (3)

• The role of cosmic rays on magnetic field diffusion and the formation of protostellar discs
• Power requirements for cosmic ray propagation models involving re-acceleration and a comment on second order Fermi acceleration theory
• Superdiffusive Stochastic Fermi Acceleration in Space and Energy