Helium stratification in HD 145792: a new Helium strong star

TL;DR

This study reclassifies HD 145792 as a helium-strong star with helium stratification and provides detailed atmospheric parameters and chemical abundances using high-resolution spectroscopy.

Contribution

It is the first to determine the chemical pattern and helium stratification in HD 145792, challenging its previous classification as He weak.

Findings

HD 145792 is a helium-strong star, not He weak.

Helium is vertically stratified, decreasing in deeper layers.

Certain metals are overabundant, others are normal or slightly underabundant.

Abstract

In this paper we report on the real nature of the star HD 145792, classified as He weak in {\it ``The General Catalogue of Ap and Am stars''}. By means of FEROS@ESO1.52m high resolution spectroscopic data, we refined the atmospheric parameters of the star, obtaining: T$_{\rm eff}$ = 14400 $\pm$ 400 K, $\log g$ = 4.06 $\pm$ 0.08 and $\xi$ = 0 $^{+0.6}$ km s$^{-1}$. These values resulted always lower than those derived by different authors with pure photometric approaches. Using our values we undertook an abundance analysis with the aim to derive, for the first time, the chemical pattern of the star's atmosphere. For metals a pure LTE synthesis (ATLAS9 and SYNTHE) has been used, while for helium a hybrid approach has been preferred (ATLAS9 and SYNSPEC). The principal result of our study is that HD 145792 belongs to He strong class contrary to the previous classification. Moreover, helium seems to be vertically stratified in the atmosphere, decreasing toward deepest layers. For what that concerns metals abundances, we found the following: overabundance of oxygen, neon, silicon, phosphorus, sulfur and calcium; carbon, nitrogen, magnesium, aluminum, titanium, chromium and nickel are normal, being the discrepancies from the solar values within the experimental errors; iron resulted to be slightly underabundant.