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P/2013 P5 PANSTARRS was discovered in Aug. 2013, displaying a cometary tail,but with orbital elements typical for a member of the inner asteroid Main Belt.  We monitored the object from 2013 Aug. 30 until Oct. 05 using the CFHT, NTT,CA 1.23m, Perkins 1.8m (Lowell), and the 0.6m TRAPPIST telescopes. We measuredits nuclear radius to be r < 0.25-0.29km, and its colours g-r = 0.58+/-0.05 andr-i = 0.23+/-0.06, typical for an S-class asteroid. We failed to detect anyrotational light curve, with an amplitude < 0.05mag and a double-peakedrotation period < 20h. A detailed Finson-Probstein analysis of deep NTT andCFHT images indicated that the object was active since at least late January2013 until the time of the latest observations in 2013 September, with at leasttwo peaks of activity around 2013 June 14+/-10d and 2013 July 22+/-3d. Thechanges of activity level and the activity peaks were extremely sharp andshort, shorter than the temporal resolution of our observations (about 1d). Thedust distribution was similar during these two events, with dust grainscovering at least the 1-1000{\mu}m range. The total mass ejected in grains <1mmwas estimated to be 3.0 10$^6$kg and 2.6 10$^7$kg around the two activitypeaks.  Rotational disruption cannot be ruled out as the cause of the dust ejection.We also propose that the components of a contact binary might gently rub andproduce the observed emission. Volatile sublimation might also explain whatappears as cometary activity over a period of 8 months. However, while MainBelt comets best explained by ice sublimation are found in the outskirts of theMain Belt, where water ice is believed to be able to survive buried inmoderately large objects for the age of the solar system deeply, the presenceof volatiles in an object smaller than 300m in radius would be very surprisingin the inner asteroid belt.

Continued activity in P/2013 P5 PANSTARRS - The comet that should not be