High-resolution spectra of a sample of all known stars more luminous than MV=+6.5 and closer than 15 parsecs are being analyzed spectroscopically in order to derive their effective temperatures and surface gravities. These spectra are taken from the database of "A Spectroscopic Survey of Stars in the Solar Neighborhood". The analysis utilizes a sample of Fe I and Fe II lines. The stellar parameters derived from this analysis are compared to previously published values from various studies. A comparison of the different temperature scales will be discussed as well as the impact these differences have on chemical abundance studies of cool stars. This research is supported in part by the National Science Foundation (AST03-07534 and AST03-07532),NASA (NAG5-13175), and JPL.