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Fig. 8


Monte Carlo dust tail code simulations (red contours) compared to the VLT observations (black contours) for the input parameters derived from Rotundi et al. (2015) with a power-law exponent of the size distribution function of –2. The image dates are shown on the left side of each panel. Innermost isophotes are 4 × 10-14 solar disk units, except for panels 2014/02/28 and 2014/03/14, which have 2 × 10-14 solar disk units.

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