  We present optical time series spectroscopy of the pulsating white dwarf star
G29-38 taken at the Very Large Telescope (VLT). By measuring the variations in
brightness, Doppler shift, and line shape of each spectrum, we explore the
physics of pulsation and measure the spherical degree ($\ell$) of each stellar
pulsation mode. We measure the physical motion of the g-modes correlated with
the brightness variations for three of the eight pulsation modes in this data
set. The varying line shape reveals the spherical degree of the pulsations, an
important quantity for properly modeling the interior of the star with
asteroseismology. Performing fits to the H$\beta$, H$\gamma$, and H$\delta$
lines, we quantify the changing shape of the line and compare them to models
and previous time series spectroscopy of G~29-38. These VLT data confirm
several $\ell$ identifications and add four new values, including an additional
$\ell$=2 and a possible $\ell$=4. In total from both sets of spectroscopy of
G29-38, eleven modes now have known spherical degrees.
