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Context. Rocky planets form by the concentration of solid particles in theinner few au regions of planet-forming disks. Their chemical compositionreflects the materials in the disk available in the solid phase at the time theplanets were forming. Aims. We aim to constrain the structure and dustcomposition of the inner disk of the young star HD 144432, using an extensiveset of infrared interferometric data taken by the Very Large TelescopeInterferometer (VLTI), combining PIONIER, GRAVITY, and MATISSE observations.Methods. We introduced a new physical disk model, TGMdust, to image theinterferometric data, and to fit the disk structure and dust composition. Wealso performed equilibrium condensation calculations with GGchem. Results. Ourbest-fit model has three disk zones with ring-like structures at 0.15, 1.3, and4.1 au. Assuming that the dark regions in the disk at ~0.9 au and at ~3 au aregaps opened by planets, we estimate the masses of the putative gap-openingplanets to be around a Jupiter mass. We find evidence for an optically thinemission ($\tau<0.4$) from the inner two disk zones ($r<4$ au) at $\lambda>3\\mu$m. Our silicate compositional fits confirm radial mineralogy gradients. Toidentify the dust component responsible for the infrared continuum emission, weexplore two cases for the dust composition, one with a silicate+iron mixtureand the other with a silicate+carbon one. We find that the iron-rich modelprovides a better fit to the spectral energy distribution. Conclusions. Wepropose that in the warm inner regions ($r<5$ au) of typical planet-formingdisks, most if not all carbon is in the gas phase, while iron and iron sulfidegrains are major constituents of the solid mixture along with forsterite andenstatite. Our analysis demonstrates the need for detailed studies of the dustin inner disks with new mid-infrared instruments such as MATISSE and JWST/MIRI.

Mid-infrared evidence for iron-rich dust in the multi-ringed inner disk of HD 144432