El período orbital de la binaria simbiótica AE Arae

We present an analysis of visual photometric and spectroscopic observations of the symbiotic binary AE Ara. The visual light curve shows ~ 830-day periodicity. We argue that the periodic photometric changes and the related changes in the optical HI and HeI emission line fluxes as well as changes in the relative TiO band depths are due to occultation of the hot emission region by the cool giant, and associate the 830-day period with the orbital period of AE Ara. We also derive and discuss the physical parameters of the binary components. AE Ara is composed of an M 5.5 III giant similar to the galactic bulge M giants, and hot luminous companion similar to the subluminous W-R/WC stars detected in some planetary nebulae. The system is embedded in an ionized nebula presumably formed from the wind expelled by the hot component.