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 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. © 2010. The Astronomical Society of the Pacific. All rights reserved.
Publication Source (Journal or Book title)
Publications of the Astronomical Society of the Pacific
Touhami, Y., Richardson, N., Gies, D., Schaefer, G., Boyajian, T., Williams, S., Grundstrom, E., Mcswain, M., Clemens, D., & Taylor, B. (2010). Spectral energy distributions of be and other massive stars. Publications of the Astronomical Society of the Pacific, 122 (890), 379-395. https://doi.org/10.1086/652009