Monte-Carlo radiative transfer simulation of the circumstellar disk of the Herbig Ae star HD 144432

TL;DR

This study uses Monte-Carlo radiative transfer simulations to model the dust distribution in the protoplanetary disk of HD 144432, revealing a gap and complex inner disk structure relevant to disk evolution and planet formation.

Contribution

It introduces a detailed two-dimensional radiative transfer model of HD 144432's disk, identifying a gap and inner disk components with new insights into their optical properties.

Findings

Identification of an inner optically thin component at 0.21-0.32 AU

Detection of a gap-like discontinuity in the disk

Evidence for coexisting optically thin and thick components in the inner region

Abstract

Studies of pre-transitional disks, with a gap region between the inner infrared-emitting region and the outer disk, are important to improving our understanding of disk evolution and planet formation. Previous infrared interferometric observations have shown hints of a gap region in the protoplanetary disk around the Herbig Ae star HD~144432. We study the dust distribution around this star with two-dimensional radiative transfer modeling. We compare the model predictions obtained via the Monte-Carlo radiative transfer code RADMC-3D with infrared interferometric observations and the {\SED} of HD~144432. The best-fit model that we found consists of an inner optically thin component at $0.21\enDash0.32~\AU$ and an optically thick outer disk at $1.4\enDash10~\AU$. We also found an alternative model in which the inner sub-AU region consists of an optically thin and an optically thick component. Our modeling suggests an optically thin component exists in the inner sub-AU region, although an optically thick component may coexist in the same region. Our modeling also suggests a gap-like discontinuity in the disk of HD~144432.