Spectral Energy Distributions of Be and Other Massive Stars

We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high–angular-resolution interferometric observations to model the density structure and sky orientation of the gas surround...

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Bibliographic Details
Published in:Publications of the Astronomical Society of the Pacific 2010-04, Vol.122 (890), p.379-395
Main Authors: Touhami, Y., Richardson, N. D., Gies, D. R., Schaefer, G. H., Boyajian, T. S., Williams, S. J., Grundstrom, E. D., McSwain, M. V., Clemens, D. P., Taylor, B.
Format: Article
Language:English
Subjects:
Astronomy
Be stars
Earth, ocean, space
Emission line stars
Emission spectra
Exact sciences and technology
Infrared excess
Rotational spectra
Spectral energy distribution
Spectral resolution
Stars
Stellar spectra
Wavelengths
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Summary:We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high–angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.
ISSN:0004-6280
1538-3873
DOI:10.1086/652009