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Fig. 20


Model fits to the [Ca II] λ 7291 profiles corresponding to the FEROS spectra (2014 and December 2015 data, top and bottom panels, respectively). The computed profiles (in red line) were obtained combining different emission structures with different projected Keplerian rotational velocities (see Table 1). The [Ca II] λ 7291 line from November 2015 FEROS data could not be modelled since it is very noisy.

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