Fig. 5
Comparison of the observed first (8498 Å) and second (8542 Å) Ca ii IRT line profiles (blue dashed line) with a photospheric model (red solid line). The model was created using the SPECTRUM program (Gray & Corbally 1994) based on a Kurucz stellar atmosphere model for Teff = 5000 K, log g = 4.5, and solar metallicity (Castelli & Kurucz 2004).
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