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Fig. 6


Comparison between the synthetic profile of C IV doublet resulting from summing all the line profiles derived from the simulations of a train of blobs (black) and the observed spectrum of TW Hya analyzed by Ardila et al. (2013; red). We assumed an angle between the line of sight and the axis of the accretion column of 65 deg to fit the velocity shift of the peak emission of the observed line. The profiles are normalized to their maximum value. The dotted gray lines represent the rest positions of the doublet.

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