Abstract
In this contribution I review how optical interferometry has contributed to shaping our understanding of the class of Herbig Ae/Be stars and of their associated circumstellar disks. I discuss the evidence for an optically-thin cavity in the inner few astronomical units (au) and a “puffed-up rim” near the dust sublimation radius and how these observations helped to establish the current generation of irradiated disk models. Multi-wavelength interferometric observations also revealed systems with clear signatures of grain growth and dynamically-cleared disk gaps, tracing important stages of disk evolution and of ongoing planet formation. I discuss the new opportunities provided by spectro-interferometry, which enables detailed studies on the gas distribution and velocity field on sub-au scales, resulting in constrains on the accretion properties of the system and the disk excitation structure. Finally, I outline some of the open questions and loose ends in current interferometric studies, and how these might point towards new disk physics.
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