Fig. 2
Left: rates of period change of ℓ = 1g modes versus the pulsation periods, corresponding to WD models characterized by an effective temperature of Teff ~ 9000 K and different stellar masses (0.1554 ≤ M⋆/M⊙ ≤ 0.4352). Middle: same as in left panel, but for ℓ = 1p modes. Right: same as in left panel, but for radial (ℓ = 0) modes.
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