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V1184 Tau (CB 34V) lies in the field of the Bok globule CB 34 and wasdiscovered as a large amplitude variable in 1993. According to the firsthypothesis of the variability of the star, it is a FU Orionis candidate eruptedbetween 1951 and 1993. During subsequent observations, the star manifests largeamplitude variability interpreted as obscuration from circumstellar clouds ofdust. We included V1184 Tau (CB 34V) in our target list of highly variablepre-main-sequence stars to determine the reasons for the variations in thebrightness of this object. Data from BVRI photometric observations of the youngstellar object V1184 Tau, obtained in the period 2008-2015, are presented inthe paper. These data are a continuation of our optical photometric monitoringof the star began in 2000 and continuing to date. The photometric observationsof V1184 Tau were performed in two observatories with two medium-sized and twosmall telescopes. Our results indicate that during periods of maximum light thestar shows characteristics typical of T Tauri stars. During the observed deepminimum in brightness, however, V1184 Tau is rather similar to UX Orionisobjects. The deep drop in brightness began in 2003 ended in 2015 as the starhas returned to maximum light. The light curve during the drop is obviouslyasymmetric as the decrease in brightness lasts two times longer than the rise.The observed colour reverse on the colour-magnitude diagrams is alsoconfirmation of obscuration from circumstellar clouds of dust as a reason forthe large amplitude variability in the brightness.

The PMS star V1184 Tau (CB 34V) at the end of prolonged eclipse