UX Ori Stars Eclipses by Large-Scale Disc Perturbations

TL;DR

This study models how large-scale disc perturbations around UX Ori stars affect their eclipses, polarization, and color indices, revealing deeper eclipses and variable polarization patterns compared to compact cloud models.

Contribution

It introduces a generalized radiative transfer model for large-scale disc perturbations, including disc puffing-up, to better understand UX Ori star eclipses and polarization behavior.

Findings

Large-scale perturbations cause deeper eclipses and higher polarization.

Disc puffing-up significantly alters polarization degree and color index.

Polarization position angle can change markedly during eclipses.

Abstract

We simulate the polarized radiative transfer in vicinities of the UX Ori type stars during their minima. Our model of an eclipse by an extended disc perturbation generalizes the compact gas-dust cloud eclipse model. We apply the radiative transfer method based on enumeration using the directions grid to model the influence of the perturbation extensions along azimuth and radius on the eclipse depth and parameters of the linear polarization. We investigate eclipses both for the flared disc and for the disc with a puffing-up in the dust sublimation zone. The puffing-up is obtained by adding a disc wind to the model. Comparison with a compact cloud eclipse model reveals that the eclipse by a large-scale azimuthally extended perturbation may be significantly deeper and show a greater linear polarization degree. We also demonstrate that the perturbation extension together with the disc puffing-up can strongly affect the degree of polarization and colour index of the star during the eclipse. The position angle of the linear polarization may also change markedly during and after an eclipse by a large scale perturbation for the model with a puffed-up inner rim. Also, in this model, the maximum degree of the linear polarization can be achieved not at the brightness minimum but closer to the end of the eclipse. We discuss the modelling results in the context of the photopolarimetric observations of UX Ori stars.