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Fig. 1


Location of the known ELMVs (big red circles) along with the other several classes of pulsating WD stars (dots of different colors) in the log Teff−log g plane. In parenthesis we include the number of known members of each class. Two post-VLTP (very late thermal pulse) evolutionary tracks for H-deficient WDs and two evolutionary tracks for low-mass He-core WDs are plotted for reference. Also shown is the theoretical blue edge of the instability strip for the GW Vir stars (Córsico et al. 2006), the hot DAV stars, (Shibahashi 2013), V777 Her stars (Córsico et al. 2009a), the DQV stars (Córsico et al. 2009b), the ZZ Ceti stars (Fontaine & Brassard 2008), and the pulsating low-mass WDs (Hermes et al. 2013a).

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