Scattering linear polarization of late-type active stars

TL;DR

This study models the intrinsic linear polarization of late-type active stars caused by star spots, aiming to aid in star and exoplanet atmosphere characterization through polarimetric observations.

Contribution

The paper introduces a new simulation code to estimate stellar polarization considering various spot configurations and stellar parameters, advancing star spot and exoplanet studies.

Findings

Polarization increases with spot coverage and temperature contrast.

Polar spots and active latitudes significantly influence polarization signals.

The model predicts polarization levels that could impact exoplanet atmosphere studies.

Abstract

Many active stars are covered in spots, much more so than the Sun, as indicated by spectroscopic and photometric observations. It has been predicted that star spots induce non-zero intrinsic linear polarization by breaking the visible stellar disk symmetry. Although small, this effect might be useful for star spot studies, and it is particularly significant for a future polarimetric atmosphere characterization of exoplanets orbiting active host stars. Using models for a center-to-limb variation of the intensity and polarization in presence of continuum scattering and adopting a simplified two-temperature photosphere model, we aim to estimate the intrinsic linear polarization for late-type stars of different gravity, effective temperature, and spottedness. We developed a code that simulates various spot configurations or uses arbitrary surface maps, performs numerical disk integration, and builds Stokes parameter phase curves for a star over a rotation period for a selected wavelength. It allows estimating minimum and maximum polarization values for a given set of stellar parameters and spot coverages. Based on assumptions about photosphere-to-spot temperature contrasts and spot size distributions, we calculate the linear polarization for late-type stars with $T_{\rm eff}$ = 3500 K - 6000 K, log$g$ = 1.0 - 5.0, using the plane-parallel and spherical atmosphere models. Employing random spot surface distribution, we analyze the relation between spot coverage and polarization and determine the influence of different input parameters on results. Furthermore, we consider spot configurations with polar spots and active latitudes and longitudes.