Fig. 1.

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Δν − ΔΠ1 relation of RGB stars studied by V16. Only stars with ΔΠ1 < 130 s are represented in order to remove the contribution from core-He burning giants. Stars are color-coded by their mass, obtained from seismic scaling relations. The thick black dashed line indicates the average RGB sequence as obtained from observations (see Sect. 5.1).
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