¹ Astronomical Institute of the Charles University, V Holesovickach 2, CZ-180 00 Praha 8, Czech Republic
² Astronomical Institute of the Academy of Sciences, CZ-251 65 Ondrejov, Czech Republic,
 e-mail:hec(bozic)@sunstel.asu.cas.cz
³ Hvar Observatory, Faculty of Geodesy, Kaciceva 26, 10000 Zagreb, Croatia
 e-mail:hbozic(dsudar,domago)@hvar.geof.hr
⁴ Erindale College and Department of Astronomy, University of Toronto, Mississauga, ON L5LIC6, Canada
 e-mail:jpercy@erin.utoronto.ca
⁵ Department of Physics and Astronomy, University of Victoria. P.O. Box 3055 STN CSC, Victoria, B.C., Canada V8W 3P6
 yang@uvastro.phys.uvic.ca
⁶ National Astronomical Observatory, Rozhen, Bulgaria and Isaak Newton Institute of Chile, Bulgarian Branch
 e-mail:liliev@libra.astro.bas.bg
⁷ Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
 e-mail:hlin@class1.bao.ac.cn
⁸ Association des Utilisateurs de Detecteurs Electroniques (AUDE), 28, rue du Pic du Midi, F-31130 Quint-Fonsegrives, France
 e-mail:christian.buil@cnew.fr
Dept. of Astronomy, University of Guanajuato, 36000 Guanajuato, GTO, Mexico
 e-mail:eenens@astro.ugto.mx

An analysis of numerous homogenized UBV photoelectric observations and red spectra of the Be star V832 Cyg from several observatories led to the following principal findings:
1. Pronounced long-term light and colour variations of V832 Cyg result from a combination of two effects: from the gradual formation of a new Be envelope, and from an asymmetry and a slow revolution of the envelope (or its one-armed oscillation). The colour variations associated with the envelope formation are characterized by a positive correlation between brightness and emission strength, typical for stars which are not seen roughly equator-on.
2. The V magnitude observations prewhitened for the long-term changes follow a sinusoidal orbital light curve with a small amplitude and a period of 28^d.1971 which is derived from observations spanning 43 years. This independently confirms a 12-year old suggestion that the star is a spectroscopic binary with a 29-d period. V832 Cyg thus becomes the fifth known Be star with cyclic long-term V/R variations, the duplicity of which has been proven, the four other cases being Tau, V923 Aql, Cas and X Per. Therefore, the hypothesis that the long-term V/R variations may arise due to the attractive force of the binary companion at certain phases of the envelope formation is still worth considering as a viable alternative to the model of one-armed oscillation.
3. We have shown that the RV and V/R variations of the H and He I 6678 emission lines are all roughly in phase. In particular, the He I 6678 emission also moves with the Be primary which differs from what was found for another Be binary, Per.
4. We derived the orbital elements and found that in spite of the remaining uncertainties, the basic physical properties of the 28^d.2 binary are well constrained.
5. The light minimum of the orbital light curve occurs at elongation when the Be star is approaching us and the object becomes bluest in (B - V) and reddest in (U - B) at the same time. This may indicate that a part of the optically thick regions of the envelope is eclipsed at these orbital phases.

Accepted by A&A
Preprints from hec@sunstel.asu.cas.cz
or on the web at ftp://astro.troja.mff.cuni.cz/pub/hec/zarf21.ps