Fundamental parameters of bright Ap stars from wide-range energy distributions and advanced atmospheric models

TL;DR

This study derives accurate stellar parameters for three bright Ap stars using advanced atmospheric models, energy distributions, and precise parallaxes, overcoming challenges posed by magnetic fields and chemical peculiarities.

Contribution

It introduces a comprehensive method combining observed energy distributions, high-resolution spectroscopy, and advanced models to determine parameters of magnetic chemically peculiar stars.

Findings

Accurate stellar radii consistent with interferometric measurements.

Effective temperatures and gravities derived from combined spectroscopic and photometric data.

Self-consistent atmospheric models with stratification profiles constructed.

Abstract

As a well-established procedure for the vast majority of normal main-sequence stars, determination of atmospheric and stellar parameters turns to be a challenging process in case of magnetic chemically peculiar stars. Inhomogeneous distribution of chemical elements and strong magnetic fields make most of the standard photometric and spectroscopic calibrations inapplicable for this class of stars. In this work we make use of available observed energy distributions calibrated to absolute units, stellar parallaxes, high-resolution spectroscopic observations, and advanced stellar atmosphere models to derive parameters of three bright Ap stars: 33Lib, gammaEqu, and betaCrB. Model atmospheres and fluxes were computed with the LLmodels code. Synth3 and Synthmag codes were used to compute profiles of individual spectral lines involved in abundance analysis. For each of the stars, we construct a self-consistent atmospheric models assuming normal and depleted helium compositions and derive empirically stratification profiles of certain elements. The effective temperatures and surface gravities are found from the simultaneous fit to spectroscopic, photometric, and spectrophotometric observations calibrated to absolute units. We show that using advanced model atmospheres and accurate stellar parallaxes allows one to derive stellar radii with high accuracy, and these are consistent with those obtained from independent but more complicated interferometric observations.