Project VeSElkA: Analysis of Balmer line profiles in slowly rotating chemically peculiar stars

TL;DR

This study estimates fundamental stellar parameters for chemically peculiar stars using Balmer line profiles and stellar atmosphere models, providing new data for four stars and insights into their atmospheric properties.

Contribution

First determination of effective temperature and gravity for four chemically peculiar stars using Balmer line fitting with PHOENIX models.

Findings

Effective temperatures and gravities for four stars are determined for the first time.

Stellar atmosphere models are used to fit Balmer line profiles for parameter estimation.

Physical characteristics of 16 stars are discussed, setting the stage for abundance stratification studies.

Abstract

We present results for the estimation of gravity, effective temperature, and radial velocity of poorly studied chemically peculiar stars recently observed with the spectropolarimeter Echelle SpectroPolarimetric Device for Observations of Stars at the Canada-France-Hawaii Telescope in the frame of the Vertical Stratification of Element Abundances project. The effective temperature and surface gravity values are determined for the very first time for four of the stars from our sample (HD23878, HD83373, HD95608, and HD164584). Grids of stellar atmosphere models with the corresponding fluxes have been calculated using version 15 of the PHOENIX code for effective temperatures in the range of 5000-15,000 K, for the logarithm of surface gravities in the range of 3.0-4.5 and for the metallicities from -1.0 to +1.5. We used these fluxes to fit the Balmer line profiles employing the code FITSB2 that produces estimates of the effective temperature, gravity, and radial velocity for each star. When possible, our results are compared to those previously published. The physical characteristics of 16 program stars are discussed with the future aim to study the abundance anomalies of chemical species and the possible vertical abundance stratification in their stellar atmosphere.