Spectral Energy Distributions of Be and Other Massive Stars

Abstract

We present spectrophotometric data from 0.4 to 4.2 microns 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 H-alpha 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, PASP, 122, 379

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• A simple connection between the near- and mid-infrared emission of galaxies and their star-formation rates
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• The Circumstellar Disk of the Be Star $o$~Aquarii
• Dusty OB Stars in the Small Magellanic Cloud - I: Optical Spectroscopy Reveals Predominantly Main-Sequence OB Stars
• The H-band Emitting Region of the Luminous Blue Variable P Cygni: Spectrophotometry and Interferometry of the Wind
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• Fluorescent Fe K line emission of gamma Cas stars I. Do gamma Cas stars host propelling neutron stars?
• Evolutionary status of isolated B[e] stars
• B stars seen at high resolution by XMM-Newton
• The disk physical conditions of 48 Persei constrained by contemporaneous Hα spectroscopy and interferometry