Faculae cancel out on the surfaces of active Suns

TL;DR

This paper uses a surface flux transport model to show that magnetic flux cancellation affects the observed relationship between spots and faculae on the Sun and other stars, improving stellar activity correction methods.

Contribution

It introduces a model explaining how magnetic flux cancellation influences the relative coverage of spots and faculae, aiding better stellar activity mitigation.

Findings

Faculae cancellation leads to faster spot coverage increase with activity.

The model explains the solar spot-faculae coverage relationship.

Extension of the model to active stars improves exoplanet characterization.

Abstract

Surfaces of the Sun and other cool stars are filled with magnetic fields, which are either seen as dark compact spots or more diffuse bright structures like faculae. Both hamper detection and characterisation of exoplanets, affecting stellar brightness and spectra, as well as transmission spectra. However, the expected facular and spot signals in stellar data are quite different, for instance they have distinct temporal and spectral profiles. Consequently, corrections of stellar data for magnetic activity can greatly benefit from the insight on whether the stellar signal is dominated by spots or faculae. Here, we utilise a surface flux transport model (SFTM) to show that more effective cancellation of diffuse magnetic flux associated with faculae leads to spot area coverages increasing faster with stellar magnetic activity than that by faculae. Our calculations explain the observed dependence between solar spot and facular area coverages and allow its extension to stars more active than the Sun. This extension enables anticipating the properties of stellar signal and its more reliable mitigation, leading to a more accurate characterisation of exoplanets and their atmospheres.