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Collisional growth of dust occurs in all regions of protoplanetary disks withcertain materials dominating between various condensation lines. The stickingproperties of the prevalent dust species depend on the specific temperatures.The inner disk is the realm of silicates spanning a wide range of temperaturesfrom room temperature up to sublimation beyond $1500\,\mathrm{K}$. For thefirst time, we carried out laboratory collision experiments with hot levitatedbasalt dust aggregates of $1\, \rm mm$ in size. The aggregates are compact witha filling factor of $0.37 \pm 0.06$. The constituent grains have a wide sizedistribution that peaks at about $0.6\,\mu \mathrm{m}$. Temperatures in theexperiments are varied between approximately $600\,\mathrm{K}$ and$1100\,\mathrm{K}$. Collisions are slow with velocities between$0.002\,\mathrm{m}\,\mathrm{s}^{-1}$ and $0.15\,\mathrm{m}\,\mathrm{s}^{-1}$,i.e., relevant for protoplanetary disks. Aside from variations of thecoefficients of restitution due to varying collision velocities, theexperiments show low sticking probability below $900\,\mathrm{K}$ and anincreasing sticking probability starting at $900\,\mathrm{K}$. This impliesthat dust can grow to larger size in hot regions, which might change planetformation. One scenario is an enhanced probability for local planetesimalformation. Another scenario is a reduction of planetesimal formation as largergrains are more readily removed as a consequence of radial drift. However, theincreased growth at high temperatures likely changes planetesimal formation oneway or the other.

Onset of planet formation in the warm inner disk -- Colliding dust aggregates at high temperatures