  We present further photometric observations of the unusual F0 V star 9
Aurigae and present evidence that this star's radial velocity, spectroscopic
line widths and line depths are also variable with the same frequencies as the
photometric data ($f_1 \approx 0.795$ and $f_2 \approx 0.345$ d$^{-1}$). The
phases of these sinusoids are stable over time scales of longer than one year,
though the amplitudes can vary, making the prediction of photometric behavior
impossible. Given that a variety of other explanations have already been
discounted (e.g. interactions with a close companion, the existence of a lumpy,
orbiting ring of dust, or star spots) and that these variations occur on time
scales an order of magnitude slower than the fundamental radial pulsation
period, we have very strong evidence that 9 Aurigae exhibits non-radial {\it
g}-mode pulsations. Since the power spectrum of the radial velocity data shows
frequency $f_2$ but does not clearly show $f_1$, the present data suggest that
$f_2$ is associated with a low degree spherical harmonic ($\ell$ = 1 or 2),
while $f_1$ is associated with a higher degree harmonic. 9 Aurigae, along with
such stars as $\gamma$ Doradus, HD 224638, HD 224945, and HD 164615, appear to
constitute a new class of pulsating variables. These stars are to be found at
or beyond the cool edge of the Cepheid instability strip in the HR Diagram.
Prior to this, only much hotter stars have been shown to exhibit non-radial
{\it g}-modes.
