Ultraviolet Spectrophotometry of Variable Early-Type Be and B stars Derived from High-Resolution IUE Data

High-dispersion IUE data encode significant information about aggregate line absorptions that cannot be conveniently extracted from individual stellar spectra. Herein we apply a new technique in which fluxes from each echelle order of a short-wavelength IUE spectrum are binned together to construct low-resolution spectra of a rapidly varying B or Be star. The division of binned spectra obtained during a “bright-star” phase by spectra from a “faint-star” phase leads to a ratioed spectrum which contains information about the mechanism responsible for a star’s variability. The most likely candidate mechanisms are either the periodic or episodic occultations of the star by ejected matter or a change in photospheric structure, e.g. from pulsation. We model the variations caused by these mechanism by means of model atmosphere and absorbing-slab codes. Line absorptions strength changes are rather sensitive to physical conditions in circumstellar shells and “clouds” at temperatures of 8,000–13,000 K, which is the regime expected for circumstellar structures of early B stars. To demonstrate proofs of concept, we construct spectral ratios for circumstellar structures associated with flux variability in various Be stars: (1) VelaX-1 has a bow-shock wind trailing its neutron star companion; at successive phases and hence in different sectors, the wind exhibits spectrophotometric signatures of a 13,000K or 26,000K medium, (2) 88Her undergoes episodic “outbursts” during which its UV flux fades, followed a year later by a dimming at visible wavelengths as well; the ratioed spectrum indicates the “phase lag” is a result of a nearly gray opacity that dominates all wavelengths as the shell expands from the star and cools, permitting the absorptions in the visible to “catch up” to those in the UV, and (3) ζ Tau and 60Cyg exhibit periodic