Gaps in Protoplanetary Disks as Signatures of Planets: III. Polarization

TL;DR

Polarimetric imaging of protoplanetary disks reveals how inclination and gaps affect observed polarization, aiding interpretation of disk structures and dust properties when combined with total intensity data.

Contribution

This study analyzes how disk inclination and planetary gaps influence polarized light images, improving interpretation of disk features and dust characteristics.

Findings

Inclination distorts isophotes, mimicking higher eccentricity or inclination.

Gap contrast varies with polarization, affecting detectability.

Polarized images alone are insufficient; combined with total intensity data enhances understanding.

Abstract

Polarimetric observations of T Tauri and Herbig Ae/Be stars are a powerful way to image protoplanetary disks. However, interpretation of these images is difficult because the degree of polarization is highly sensitive to the angle of scattering of stellar light off the disk surface. We examine how disks with and without gaps created by planets appear in scattered polarized light as a function of inclination angle. Isophotes of inclined disks without gaps are distorted in polarized light, giving the appearance that the disks are more eccentric or more highly inclined than they truly are. Apparent gap locations are unaffected by polarization, but the gap contrast changes. In face-on disks with gaps, we find that the brightened far edge of the gap scatters less polarized light than the rest of the disk, resulting in slightly decreased contrast between the gap trough and the brightened far edge. In inclined disks, gaps can take on the appearance of being localized "holes" in brightness rather than full axisymmetric structures. Photocenter offsets along the minor axis of the disk in both total intensity and polarized intensity images can be readily explained by the finite thickness of the disk. Alone, polarized scattered light images of disks do not necessarily reveal intrinsic disk structure. However, when combined with total intensity images, the orientation of the disk can be deduced and much can be learned about disk structure and dust properties.