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Fig. 3


Characteristic heating timescales in the inner disc region for a solar nebula model (from Sect. 6.1) at disc ages of 1 Ma (solid line) and 2 Ma (dashed line). Shown are the mixing timescales in horizontal and vertical direction, τhor and τvert, respectively, and the timescale for heating of disc material, τheat, due to inward drift by accretion.

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