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The periodicity of 5.5 years for some observational events occurring in EtaCarinae manifests itself across a large wavelength range and has beenassociated with its binary nature. These events are supposed to occur when thebinary components are close to periastron. To detect the previous periastronpassage of Eta Car in 2003, we started an intensive, ground-based, optical,photometric observing campaign. We continued observing the object to monitorits photometric behavior and variability across the entire orbital cycle. Ourobservation program consisted of daily differential photometry from CCD images,which were acquired using a 0.8 m telescope and a standard BVRI filter set atLa Plata Observatory. The photometry includes the central object and thesurrounding Homunculus nebula. We present up-to-date results of our observingprogram, including homogeneous photometric data collected between 2003 and2008. Our observations demonstrated that Eta Car has continued increasing inbrightness at a constant rate since 1998. In 2006, it reached its brightestmagnitude (V ~ 4.7) since about 1860s. The object then suddenly reverted itsbrightening trend, fading to V = 5.0 at the beginning of 2007, and hasmaintained a quite steady state since then. We continue the photometricmonitoring of Eta Car in anticipation of the next "periastron passage",predicted to occur at the beginning of 2009.

Long-Term Optical Monitoring of Eta Carinae. Multiband light curves for a complete orbital period