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A warm/hot dust component (at temperature $>$ 300K) has been detected around$\sim$ 20% of stars. This component is called "exozodiacal dust" as it presentssimilarities with the zodiacal dust detected in our Solar System, even thoughits physical properties and spatial distribution can be significantlydifferent. Understanding the origin and evolution of this dust is of crucialimportance, not only because its presence could hamper future detections ofEarth-like planets in their habitable zones, but also because it can provideinvaluable information about the inner regions of planetary systems. In thisreview, we present a detailed overview of the observational techniques used inthe detection and characterisation of exozodiacal dust clouds ("exozodis") andthe results they have yielded so far, in particular regarding the incidencerate of exozodis as a function of crucial parameters such as stellar type andage, or the presence of an outer cold debris disc. We also present theimportant constraints that have been obtained, on dust size distribution andspatial location, by using state-of-the-art radiation transfer models on someof these systems. Finally, we investigate the crucial issue of how to explainthe presence of exozodiacal dust around so many stars (regardless of theirages) despite the fact that such dust so close to its host star shoulddisappear rapidly due to the coupled effect of collisions and stellar radiationpressure. Several potential mechanisms have been proposed to solve this paradoxand are reviewed in detail in this paper. The review finishes by presenting thefuture of this growing field.

Exozodiacal clouds: Hot and warm dust around main sequence stars