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A reliable determination of the basic physical properties and variabilitypatterns of hot emission-line stars is important for understanding the Bephenomenon and ultimately, the evolutionary stage of Be stars. This study isdevoted to one of the most remarkable Be stars, V1294 Aql = HD 184279. Wecollected and analysed spectroscopic and photometric observations covering atime interval of about 25000 d (68 yr). We present evidence that the object isa single-line 192.9 d spectroscopic binary and estimate that the secondaryprobably is a hot compact object with a mass of about 1.1-1.2 solar masses. Wefound and documented very complicated orbital and long-term spectral, light,and colour variations, which must arise from a combination of several distinctvariability patterns. Attempts at modelling them are planned for a follow-upstudy. We place the time behaviour of V1294 Aql into context with variationsknown for some other systematically studied Be stars and discuss the currentideas about the nature of the Be phenomenon.

V1294 Aql = HD 184279: A bad boy among Be stars or an important clue to the Be phenomenon?