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We study the sub-AU-scale circumstellar environment of the Herbig Ae starHD144432 with near-infrared (NIR) VLTI/AMBER observations to investigate thestructure of its inner dust disk. The interferometric observations were carriedout with the AMBER instrument in the H and K band. We interpret the measured H-and K-band visibilities, the near- and mid-infrared visibilities from theliterature, and the SED of HD144432 by using geometric ring models andring-shaped temperature-gradient disk models with power-law temperaturedistributions. We derived a K-band ring-fit radius of 0.17 \pm 0.01 AU and anH-band radius of 0.18 \pm 0.01 AU (for a distance of 145 pc). This measuredK-band radius of \sim0.17 AU lies in the range between the dust sublimationradius of \sim0.13 AU (predicted for a dust sublimation temperature of 1500 Kand gray dust) and the prediction of models including backwarming (\sim0.27AU). We found that an additional extended halo component is required in boththe geometric and temperature-gradient modeling. In the best temperature-gradient model, the disk consists of two components. The inner part of the diskis a thin ring with an inner radius of \sim0.21 AU, a temperature of \sim1600K, and a ring thickness \sim0.02 AU. The outer part extends from \sim1 AU to\sim10 AU with an inner temperature of \sim400 K. We find that the disk isnearly face-on with an inclination angle of < 28 degree. Ourtemperature-gradient modeling suggests that the NIR excess is dominated byemission from a narrow, bright rim located at the dust sublimation radius,while an extended halo component contributes \sim6% to the total flux at 2{\mu}m. The MIR model emission has a two-component structure with \sim20% fluxfrom the inner ring and the rest from the outer part. This two-componentstructure suggests a disk gap, which is possibly caused by the shadow of apuffed-up inner rim.

Near-infrared interferometric observation of the Herbig Ae star HD144432 with VLTI/AMBER