  Exo-zodiacal dust, exozodi for short, is warm (~300K) or hot (up to ~2000K)
dust found in the inner regions of planetary systems around main sequence
stars. In analogy to our own zodiacal dust, it may be located in or near the
habitable zone or closer in, down to the dust sublimation distance. The study
of the properties, distribution, and evolution of exozodis can inform about the
architecture and dynamics of the innermost regions of planetary systems, close
to their habitable zones. On the other hand, the presence of large amounts of
exo-zodiacal dust may be an obstacle for future space missions aiming to image
Earth-like exoplanets. The dust can be the most luminous component of
extrasolar planetary systems, but predominantly emits in the near- to
mid-infrared where it is outshone by the host star. Interferometry provides a
unique method of separating the dusty from the stellar emission. We discuss the
prospects of exozodi observations with the next generation VLTI instruments and
summarize critical instrument specifications.
