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Long-lived massive magnetars are expected to be remnants of some binaryneutron star (BNS) mergers. In this paper, we argue that the magnetic poweredflaring activities of these merged magnetars would occur dominantly in theirearly millisecond-period-spin phase, which is in the timescale of days. Suchflares endure significant absorption by the ejecta from the BNS collision, andtheir detectable energy range is from 0.1-10 MeV, in a time-lag of $\sim$ daysafter the merger events indicated by the gravitational wave chirps. We estimatethe rate of such flares in different energy ranges, and find that there couldhave been ~0.1-10 cases detected by Fermi/GBM. A careful search for $\sim10$milliseconds spin period modulation in weak short gamma-ray bursts (GRBs) mayidentify them from the archival data. The next generation MeV detectors coulddetect them at a mildly higher rate. The recent report on theQuasi-Period-Oscillation found in two BASTE GRBs should not be considered ascases of such flares, for they were detected in a lower energy range and with amuch shorter period spin modulation.

Flares from merged magnetars: their prospects as a new population of gamma-ray counterparts of binary neutron star mergers