  We present long slit spectrophotometry considering the presence of thermal
inhomogeneities (t^2) of two HII regions in the Small Magellanic Cloud (SMC):
NGC 456 and NGC 460. Physical conditions and chemical abundances were
determined for three positions in NGC 456 and one position in NGC 460, first
under the assumption of uniform temperature and then allowing for the
possibility of thermal inhomogeneities. We determined t^2 values based on three
different methods: i) by comparing the temperature derived using oxygen
forbidden lines with the temperature derived using helium recombination lines,
ii) by comparing the abundances derived from oxygen forbidden lines with those
derived from oxygen recombination lines, and iii) by comparing the abundances
derived from ultraviolet carbon forbidden lines with those derived from optical
carbon recombination lines. The first two methods averaged t^2=0.067+-0.013 for
NGC 456 and t^2=0.036+-0.027 for NGC 460. These values of t^2 imply that when
gaseous abundances are determined with collisionally excited lines they are
underestimated by a factor of nearly 2. From these objects and others in the
literature, we find that in order to account for thermal inhomogeneities and
dust depletion, the O/H ratio in low metallicity HII regions should be
corrected by 0.25-0.45 dex depending on the thermal structure of the nebula, or
by 0.35 dex if such information is not available.
