Magnetic Doppler imaging considering atmospheric structure modifications due to local abundances: a luxury or a necessity?

TL;DR

This study demonstrates that magnetic Doppler imaging results are robust against atmospheric structure variations, confirming the presence of small-scale magnetic fields on Ap stars and addressing previous criticisms.

Contribution

The paper shows that neglecting atmospheric structure variations has minimal impact on magnetic mapping, validating previous magnetic Doppler imaging results.

Findings

Atmospheric structure variations negligibly affect normalized Stokes profiles.

Magnetic and chemical spot maps remain consistent when considering atmospheric variations.

Previous criticisms of magnetic Doppler imaging are based on flawed assumptions.

Abstract

Magnetic Doppler imaging is currently the most powerful method of interpreting high-resolution spectropolarimetric observations of stars. This technique has revealed the presence of unexpected small-scale magnetic fields on the surfaces of Ap stars. These studies were recently criticisied by Stift et al. (2012), who claimed that magnetic inversions are not robust and are undermined by neglecting a feedback on the Stokes line profiles from the local atmospheric structure in the regions of enhanced metal abundance. We show that Stift et al. misinterpreted published magnetic Doppler imaging results and neglected some of the most fundamental principles behind magnetic mapping. We demonstrate that the variation of atmospheric structure across the surface of a star with chemical spots affects the local continuum intensity but is negligible for the normalised local Stokes profiles. For the disk-integrated spectra of an Ap star with extreme abundance variations, we find that the assumption of a mean model atmosphere leads to moderate errors in Stokes I but is negligible for polarisation spectra. Employing a new magnetic inversion code, which incorporates the horizontal variation of atmospheric structure, we reconstructed new maps of magnetic field and Fe abundance for the Ap star alpha^2 CVn. The resulting distribution of chemical spots changes insignificantly compared to the previous modelling based on a single model atmosphere, while the magnetic field geometry does not change at all. This shows that the assertions by Stift et al. are exaggerated as a consequence of unreasonable assumptions and extrapolations, as well as methodological flaws and inconsistencies of their analysis. Our discussion proves that published magnetic inversions based on a mean stellar atmosphere are robust and reliable, and that the presence of small-scale magnetic field structures on the surfaces of Ap stars is real.