Shadows and cavities in protoplanetary disks: HD163296, HD141569A, and HD150193A in polarized light

TL;DR

This study uses high-resolution polarized light imaging to analyze the morphology of protoplanetary disks around young stars, revealing structures like broken rings and discussing factors like disk geometry and shadowing effects.

Contribution

It expands the sample of disks imaged in polarized light and links disk morphology and brightness to geometric factors such as flaring angle and shadowing.

Findings

HD163296 shows a broken ring structure with a brightness drop inward.

No extended polarized emission detected from HD141569A and HD150193A.

Disk brightness correlates with flaring angle and shadowing effects.

Abstract

The morphological evolution of dusty disks around young (few Myr-old) stars is pivotal to better understand planet formation. Since both dust grains and the global disk geometry evolve on short timescale, high-resolution imaging of a sample of objects may provide important hints towards such an evolution. We enlarge the sample of protoplanetary disks imaged in polarized light with high-resolution by observing the Herbig Ae/Be stars HD163296, HD141569A, and HD150193A. We integrate our data with previous datasets to paint a larger picture of their morphology. We report a weak detection of the disk around HD163296 in both H and Ks band. The disk is resolved as a broken ring structure with a significan surface brightness drop inward of 0.6 arcsec. No sign of extended polarized emission is detected from the disk around HD141569A and HD150193A. We propose that the absence of scattered light in the inner 0.6 arcsec around HD163296 and the non-detection of the disk around HD150193A may be due to similar geometric factors. Since these disks are known to be flat or only moderately flared, self-shadowing by the disk inner wall is the favored explanation. We show that the polarized brightness of a number of disks is indeed related to their flaring angle. Other scenarios (such as dust grain growth or interaction with icy molecules) are also discussed. On the other hand, the non-detection of HD141569A is consistent with previous datasets revealing the presence of a huge cavity in the dusty disk.