  Over two dozen early F-type variable stars have been identified which
constitute a new class of pulsating stars. These stars typically have periods
between 0.5 and 3 days with V-band variability of several hundredths of a
magnitude. Given the time scale of the variability, the pulsations would have
to be non-radial gravity-mode pulsations. The pulsational nature of some of
these stars has been proven by means of coordinated multi-longitude photometric
campaigns, radial velocity (RV) variations and line profile (LP) variations,
indicating low degree spherical harmonics ($\ell$ = 3 or less). Evidence is
that these stars are younger than 300 Myr; one would surmise that a rapid onset
of convection in their outer photospheric layers puts an end to the pulsations.
Further observation and modeling of these stars is important for our
understanding of stellar evolution, the search for $g$-modes in the Sun, and is
even relevant to the interpretation of radial velocity variations of solar-type
stars (e.g. 51 Peg) in the search for extrasolar planets.
