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Fig. 7

image

Results for our models without dust evolution, with truncated-MRN (100−250 nm) (top) and MRN (5−250 nm) (bottom) size distributions, both covered by icy mantles. Left: evolution of the fractional abundances of charged species: ions, electrons, negative charges (g-) and positive charges (g+) on grains. Centre: evolution of the dust parallel conductivity (σg), dust perpendicular conductivity (σg), ion perpendicular conductivity (σi) and Hall conductivity (σH). Scalings in powers of nH are over-plotted in dotted lines for an easier comparison of our numerical results with the asymptotic trends described in Sect. 4.1). Right: evolution of the Ohmic (ηΩ), Hall (ηH), and ambipolar diffusion (ηAD) resistivities.

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