Diffusion models for the low-frequency radio emission from the Galactic halo

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Abstract
The low-frequency drift-scan observations of the Galactic radio emission at high latitudes are discussed in the context of simple diffusion-plus-energy-loss models for the propagation of electrons away from the Galactic plane. It is shown that for certain parameters such models can reproduce the observations quite well. The halo emissivity in the region just outside the disc at the solar radius is ∼ 7000 K/kpc at 17.5 MHz. The average magnetic field in the halo must be ∼ 0.2 of that in the disc, and the diffusion mean free path about 1 pc. The full width to half-maximum of the 17.5 MHz emission is about 6 kpc.

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