Abstract:
The hot
γ
Doradus stars have multiple low frequencies characteristic of
γ
Dor or SPB variables,
but are located between the red edge of the SPB and the blue edge of the
γ
Dor instability
strips where all low-frequency modes are stable in current models of these stars. Though
δ
Sct stars also have low frequencies, there is no sign of high frequencies in hot
γ
Dor stars.
We obtained spectra to refine the locations of some of these stars in the H–R diagram and
conclude that these are, indeed, anomalous pulsating stars. The Maia variables have multiple
high frequencies characteristic of
β
Cep and
δ
Sct stars, but lie between the red edge of the
β
Cep and the blue edge of the
δ
Sct instability strips. We compile a list of all Maia candidates and
obtain spectra of two of these stars. Again, it seems likely that these are anomalous pulsating
stars which are currently not understood
