Modeling of extended atmospheres with temperatures below 40000K

TL;DR

This paper models extended stellar atmospheres with temperatures below 40,000K, focusing on emission-line objects like LBVs and ULXs, providing spectral line predictions and analysis of observed objects.

Contribution

It introduces detailed models of extended atmospheres in the 12,000-40,000K range, linking theoretical spectra with observed emission-line objects.

Findings

Model grids for hydrogen, He, Si, Fe lines generated

Equivalent width diagrams created for spectral analysis

Application to observed emission objects demonstrated

Abstract

We calculate models of extended stellar atmospheres with a temperature in the range of 12000-40000K and a mass loss rate of $10^{-6}-10^{-4} M_{\odot}$ yr$^{-1}$. A large number of objects with emission spectra, such as luminous blue variables (LBV), FeII - emission line stars, Of/late-WN stars, and even ultraluminous X-ray sources (ULXs) often have effective temperatures in this range. The paper presents the results of model grids calculating in the form of equivalent width diagrams for the selected lines of hydrogen, He, Si, and Fe, as well as the results of studies of some emission objects using the calculated models.