Selected properties of our He-core WD sequences (final cooling branch) at Teff ≈ 10 000 K: the stellar mass, the mass of H in the outer envelope, the time it takes the WD models to cool from Teff ≈ 10 000 K to ≈ 8000 K, and the occurrence (or not) of CNO flashes on the early WD cooling branch.
|M⋆/M⊙||MH/M⋆ [10-3]||τ [Gyr = 109 yr]||H-flash|
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