A Lifetime of Influence: Abstracts, Talks, and Posters
 

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van den Heuvel

  

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High-resolution near-IR spectroscopy of massive stars

M. Fernanda Nieva
Max-Planck-Institut for Astrophysics

Norbert Przybilla
Dr.-Remeis-Sternwarte Bamberg

Andreas Seifahrt
Institut for Astrophysics Goettingen

Keith Butler
Munich Observatory

Hans-Ulrich Kaufl
ESO Garching

Andreas Kaufer
ESO Santiago

Massive OB-type stars can be found in star-formation regions. They deposit energy and momentum to the interstellar medium and can ionize gas clouds through intense UV radiation. Among them, less evolved dwarfs and giants should have similar chemical composition than their parent clouds and their analysis can contribute as metallicity indicators to the understanding of star-formation processes. OB-type stars in dust-enshrouded regions are observable in the near-IR. Their high luminosity allow us to derive present-day chemical abundances of star-forming regions also at large distances. We show quantitative results from a recent analysis of high-quality spectra of early-B dwarfs and giants in the solar neighbourhood obtained with CRIRES on the VLT/UT1. The precise quantitative spectral analysis in the visual developed in the last years is extended to the near-IR for the first time at high resolution. The present work includes the identification and modelling of metal lines never resolved before and benchmark tests of spectrum synthesis, which is more challenging than in the optical because of an amplification of non-LTE effects in the near-IR. Stellar parameters are derived simultaneously from near-IR hydrogen and helium lines and metal ionization equilibria. Agreement of atmospheric parameters and chemical abundances with those obtained from the analysis in the visual is achieved, confirming the self-consistency of the quantitative analysis.