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After 26 years from the major event of 1990, in early 2016 the puzzlingsymbiotic binary MWC 560 has gone into a new and even brighter outburst. Wepresent our tight BVRI photometric monitoring of MWC 560 (451 independent runsdistributed over 357 different nights), covering the 2005-2016 interval, andthe current outburst in particoular. A stricking feature of the 2016 outbursthas been the suppression of the short term chaotic variability during the risetoward maximum brightness, and its dominance afterward with an amplitude inexcess of 0.5 mag. Similar to the 1990 event when the object remained aroundmaximum brightness for ~6 months, at the time Solar conjunction preventedfurther observations of the current outburst, MWC 560 was still around maximum,three months past reaching it. We place our observations into a long termcontex by combining with literature data to provide a complete 1928-2016lightcurve. Some strong periodicities are found to modulate the opticalphotometry of MWC 560. A period of 1860 days regulate the occourence of brightphases at BVR bands (with exactly 5.0 cycles separating the 1990 and 2016outbursts), while the peak brightness attained during bright phases seems tovary with a ~9570 days cycle. A clean 331 day periodicity modulate the I-bandlightcurve, where the emission from the M giant dominates, with a lightcurvestrongly reminiscent of an ellipsoidal distortion plus irradiation from the hotcompanion. Pros and cons of 1860 and 331 days as the system orbital period arereviewed, waiting for a spectroscopic radial velocity orbit of the M giant tosettle the question (provided the orbit is not oriented face-on).

The 2016 outburst of the unique symbiotic star MWC 560 (= V694 Mon), its long-term BVRI evolution and a marked 331 days periodicity