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Table 1.
Characteristics of the different methods considered in this work to assess the stellar mass of pulsating WDs.
| Method of derivation | Observable | Theoretical |
|---|---|---|
| Spectroscopy (MSpec) | Electromagnetic spectra | Atmosphere models (Teff, log g) |
| Evolutionary tracks (Teff − log g diagrams) | ||
| Asteroseismology (MSeis) | g-mode periods (Π) | Evolution and pulsation models |
| g-mode constant period spacing (ΔΠ) | Teff and log g to select seismological models | |
| Astrometry (MAstr) | Gaia’s parallax or distance (dBJ) | Evolutionary tracks (log(L⋆/L⊙)) |
| Gaia’s apparent magnitudes (G, GBP, GRP) | Atmosphere models (bolometric correction, BC) | |
| Spectroscopic Teff | ||
| Photometry (MPhot) | Gaia’s parallax or distance (dBJ) | Atmosphere models (synthetic fluxes, Hν) |
| Gaia’s apparent magnitudes (G, GBP, GRP) | Mass-radius relationships (M⋆ − R⋆) | |
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