Quantitative studies of the optical and UV spectra of Galactic early B supergiants I. Fundamental parameters

TL;DR

This study analyzes the optical and UV spectra of Galactic early B supergiants to determine their fundamental parameters, revealing discrepancies in UV diagnostics and suggesting revisions to stellar wind models.

Contribution

It provides a comprehensive spectroscopic analysis using CMFGEN, highlighting temperature scale reductions and challenges in modeling UV features of B supergiants.

Findings

Derived a cooler temperature scale for B supergiants.

Mass loss rates align with theoretical predictions.

Models fail to reproduce key UV spectral features.

Abstract

We undertake an optical and ultraviolet spectroscopic analysis of a sample of 20 Galactic B0 - B5 supergiants of luminosity classes Ia, Ib, Iab and II. Fundamental stellar parameters are obtained from optical diagnostics and a critical comparison of the model predictions to observed UV spectral features is made. These parameters are derived for individual stars using CMFGEN, the nLTE, line-blanketed model atmosphere code of Hillier et al., 1998. The B supergiant temperature scale derived here shows a reduction of 1000 - 3000 K compared to previous results obtained using unblanketed codes. Mass loss rate estimates are in good agreement with predicted theoretical values and all of the 20 B0 - B5 supergiants analysed show evidence for CNO processing. The observed WLR values calculated for B0 - B0.7 supergiants are larger than predicted values, whereas the reverse is true for B1 - B5 supergiants. This means that the discrepancy between observed and theoretical values cannot be resolved by adopting clumped (i.e., lower) mass loss rates, as for O stars. The most surprising result is that, although CMFGEN succeeds in reproducing the optical spectrum accurately, it fails to reproduce key UV diagnostics, such as NV and CIV P Cygni profiles, precisely. This problem arises because the models are not ionised enough and fail to reproduce the full extent of the observed absorption trough of the P Cygni profiles. These findings add further support to the need to revise the standard model of massive star winds.