  The pulsating white dwarf G29-38 possesses a dust disk and metal lines
attributed to the accretion of its disk material. \citet{vonhipg29} have
reported variability in the equivalent width of G29-38's CaII K line on the
timescale of days. We use high resolution optical spectroscopy of G29-38's CaII
K line to test this observation. Over six days spanning in June 2007 and
October 2007 we see no evidence for variability in the equivalent width of the
Ca II K line. We also sample the variability of the Ca II K line over
integrated timescales of $\sim$100-500 seconds, where errors from incomplete
coverage of pulsation modes are predicted to be $\sim$8-15%. We find that the
scatter of the equivalent widths over this time period is consistent with
measurement errors at the 7% level, slightly weaker than predicted but within
the uncertainties of predictions. Weaker Ca and Mg lines observed show no
significant variability on yearly timescales over ten years based on our data
and other high resolution spectra. We conclude that further study is warranted
to verify if the accretion onto G29-38 is variable.
