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The formation of planets is one of the major unsolved problems in modernastrophysics. Planets are believed to form out of the material in circumstellardisks known to exist around young stars, and which are a by-product of the starformation process. Therefore, the physical conditions in these disks -structure and composition as a function of stellocentric radius and verticalheight, density and temperature profiles of each component - represent theinitial conditions under which planets form. Clearly, a good understanding ofdisk structure and its time evolution are crucial to understanding planetformation, the evolution of young planetary systems (e.g. migration), and therecently discovered, and unanticipated, diversity of planetary architectures.However, the inner disk regions (interior to ~10 AU) most relevant in thecontext of planet formation are very poorly known, primarily because ofobservational challenges in spatially resolving this region. In thiscontribution we discuss opportunities for the next decade from spectrally andspatially resolved observations, and from direct imaging, using infrared longbaseline interferometry.

How and When do Planets Form? The Inner Regions of Planet Forming Disks at High Spatial and Spectral Resolution