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Fig. 3


Modeled lines, plotted in red, are fitted to observed spectral lines in black of TW Hya, VV Ser and AS 205 A. Good fits could be found for VV Ser and TW Hya using a Keplerian model with a power-law temperature profile. No good fits could be found for AS 205 A. The optimal fit to the total line profile (red) using extended emission out to 10 AU, to the narrow inner part (green) and to the outer broader wings (blue) are presented in the right figure. See text for model parameters.

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