Prevalence of SED Turndown Among Classical Be Stars: Are All Be Stars Close Binaries?
Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ ≈ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). For the remaining 31 stars, the data are inconclusive as to whether the turndown is present or not. The analysis suggests that many if not all Be stars have close companions influencing their outer disks. If confirmed to be subdwarf companions, the mass transfer spin-up scenario might explain the existence of the vast majority of classical Be stars.
Klement, Robert; Carciofi, A. C.; Rivinius, T.; Ignace, R.; Matthews, L. D.; Torstensson, K.; Gies, D.; Vieira, R. G.; Richardson, N. D.; De Souza, A. Domiciano; Bjorkman, J. E.; Hallinan, G.; Faes, D. M.; Mota, B.; Gullingsrud, A. D.; De Breuck, C.; Kervella, P.; Curé, M.; and Gunawan, D.. 2019. Prevalence of SED Turndown Among Classical Be Stars: Are All Be Stars Close Binaries?. Astrophysical Journal. Vol.885(2). https://doi.org/10.3847/1538-4357/ab48e7 ISSN: 0004-637X