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Warm debris disks are a sub-sample of the large population of debris disks,and display excess emission in the mid-IR. Around solar-type stars, very fewobjects show emission features in mid-IR spectroscopic observations, that areattributed to small, warm silicate dust grains. The origin of this warm dustcan possibly be explained either by a collision between several bodies or bytransport from an outer belt. We present and analyse new far-IR Herschel/Pacsobservations, supplemented by ground-based data in the mid-IR (VLTI/Midi andVLT/Visir), for one of these rare systems: the 10-16 Myr old debris disk aroundHD 113766 A. We improve an existing model to account for these newobservations, and better constrain the spatial distribution of the dust and itscomposition. We underline the limitations of SED modelling and the need forspatially resolved observations. We find that the system is best described byan inner disk located within the first AU, well constrained by the Midi data,and an outer disk located between 9-13 AU. In the inner dust belt, our previousfinding of Fe-rich crystalline olivine grains still holds. We do not observetime variability of the emission features over at least a 8 years time span, ina environment subjected to strong radiation pressure. The time stability of theemission features indicates that {\mu}m-sized dust grains are constantlyreplenished from the same reservoir, with a possible depletion ofsub-{\mu}m-sized grains. We suggest that the emission features may arise frommulti-composition aggregates. We discuss possible scenarios concerning theorigin of the warm dust. The compactness of the innermost regions as probed byMidi, as well as the dust composition, suggest that we are witnessing theoutcomes of (at least) one collision between partially differentiated bodies,in an environment possibly rendered unstable by terrestrial planetaryformation.

The twofold debris disk around HD 113766 A - Warm and cold dust as seen with VLTI/Midi and Herschel/Pacs