Dust grain growth and dust dispersion are essential aspects in the evolution of protoplanetary disks.
For Herbig Ae star HD 144432, we employ IR interferometry and Monte-Carlo radiative transfer to constrain the
spatial distribution and grain size of the dust.
The best-fit model that we found consists of an inner optically thin component at 0.21-0.32 AU and an
optically thick outer disk at 1.4-10 AU.
This gap region might be opened with planet-disk interaction or photoevaporation process.
The inner component are likely dominated by sub-micron dust grains.
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