We obtained high-spectral-resolution scans of (\mathrm{H}{2} \mathrm{O}^{+})emissions from Comet Austin (1990 \mathrm{~V}) using the Wisconsin dual-etalon Fabry-Perot spectrometer at the McMath-Pierce solar telescope on Kitt Peak. The 10:5 diameter field of view on the sky was centered on the comet head. From the Doppler shifts of the emissions, we determined the outflow velocities of the cometary plasma. Adopting a simple model of the ion distribution within the field of view, we determine a lower limit (\boldsymbol{\phi}{\mathrm{H}{2} 0^{+}})to the flux of (\mathrm{H}{2} \mathrm{O}^{+}) ions away from the nucleus for each night of observations. We apply a similar analysis to our previous observations of (\mathrm{H}{2} \mathrm{O}^{+}) emissions from Comet P/Halley 1986 III. Comparing (\phi{\mathrm{H}, \mathrm{O}^{+}})with the water production rate (Q_{\mathrm{H}{2} \mathrm{O}}), we find that the average ratio (\phi{\mathrm{H}{2} \mathrm{O}^{+}} / Q{\mathrm{H}{2} \mathrm{O}}) is (1.2 \times 10^{-3}) for Comet Halley (solar minimum) and (2.6 \times 0^{2}) for Comet Austin (solar maximum); these values are significantly smaller than theoretical values of the relative (\mathrm{H}{2} \mathrm{O}^{+}) production rate (Q_{\mathrm{H}{2} \mathrm{O}^{+}} / Q{\mathrm{H}_{2} \mathrm{O}} \cdot 1993) Academic Press, Inc.