Spectroscopy of B and Be stars in the diffuse stellar clusters NGC 6871 and NGC 6913

This is a study of the population of B and Be stars in the young, relatively poor, diffuse stellar clusters NGC 6871 and NGC 6913. High resolution spectra are used to study the Hα line of eleven stars in order to detect emission. Emission profiles were found for three stars in the cluster NGC 6871;...

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Bibliographic Details
Published in:Astrophysics 2009-04, Vol.52 (2), p.235-250
Main Authors: Malchenko, S. L., Tarasov, A. E.
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics
Astrophysics and Astroparticles
Astrophysics and Cosmology
Observations and Techniques
Physics
Physics and Astronomy
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Spectrum analysis
Stars & galaxies
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Summary:This is a study of the population of B and Be stars in the young, relatively poor, diffuse stellar clusters NGC 6871 and NGC 6913. High resolution spectra are used to study the Hα line of eleven stars in order to detect emission. Emission profiles were found for three stars in the cluster NGC 6871; one of these is a known WR-star and the Be-star BD +35°3956 demonstrates the transition from the B to the Be phase. Spectra of seven of the B stars revealed no traces of emission in the Hα line. During the time of our observations, the Be star V1322 Cyg in the cluster NGC 6913 had a strong emission Hα line profile with substantial variability in intensity and equivalent width. Moderate resolution spectra of seven stars in the cluster NGC 6871 over wavelengths of 4420-4960 Å and ten stars in the cluster NGC 6913 over wavelengths of 4050-5100 Å are used to classify the series of B and Be stars spectrally and to estimate their T eff and log g . It was found that three of the stars are not members of the clusters NGC 6871 or NGC 6913.
ISSN:0571-7256
1573-8191
DOI:10.1007/s10511-009-9061-9