Chemical stratification in the atmosphere of Ap star HD 133792. Regularized solution of the vertical inversion problem

TL;DR

This paper introduces a novel regularized inversion method to map vertical chemical profiles in stellar atmospheres, enabling detailed analysis of chemical stratification in Ap star HD 133792 using high-resolution spectra.

Contribution

The study develops and applies a new regularized inversion technique that reconstructs chemical stratification profiles without prior assumptions, advancing stellar atmospheric analysis methods.

Findings

HD 133792 has negligible vsini and a magnetic field of 1.1 kG.

Elements like Ca, Si, Fe show high abundance in deep layers and lower in upper atmosphere.

Mg abundance increases with height, contrasting other elements.

Abstract

High spectral resolution studies of cool Ap stars reveal conspicuous anomalies of the shape and strength of many absorption lines. This is a signature of large atmospheric chemical gradients produced by the selective radiative levitation and gravitational settling of chemical species. Here we present a new approach to mapping the vertical chemical structures in stellar atmospheres. We have developed a regularized chemical inversion procedure that uses all information available in high-resolution stellar spectra. The new technique for the first time allowed us to recover chemical profiles without making a priori assumptions about the shape of chemical distributions. We have derived average abundances and applied the vertical inversion procedure to the high-resolution VLT UVES spectra of the weakly magnetic, cool Ap star HD 133792. Our analysis yielded improved estimates of the atmospheric parameters of HD 133792. We show that this star has negligible vsini and the mean magnetic field modulus <B>=1.1+/-0.1 kG. We have derived average abundances for 43 ions and obtained vertical distributions of Ca, Si, Mg, Fe, Cr, and Sr. All these elements except Mg show high overabundance in the deep layers and solar or sub-solar composition in the upper atmosphere of HD 133792. In contrast, the Mg abundance increases with height. We find that transition from the metal-enhanced to metal-depleted zones typically occurs in a rather narrow range of depths in the atmosphere of HD 133792. Based on the derived photospheric abundances, we conclude that HD 133792 belongs to the rare group of evolved cool Ap stars, which possesses very large Fe-peak enhancement, but lacks a prominent overabundance of the rare-earth elements.