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Kilonovae are optical transients following the merger of neutron starbinaries, which are powered by the r-process heating of merger ejecta. However,if a merger remnant is a long-lived supramassive neutron star supported by itsuniform rotation, it will inject energy into the ejecta through spindown power.The energy injection can boost the peak luminosity of a kilonova by many ordersof magnitudes, thus significantly increasing the detectable volume. Therefore,even if such events are only a small fraction of the kilonovae population, theycould dominate the detection rates. However, after many years of optical skysurveys, no such event has been confirmed. In this work, we build a boostedkilonova model with rich physical details, including the description of theevolution and stability of a proto neutron star, and the energy absorptionthrough X-ray photoionization. We simulate the observation prospects and findthe only way to match the absence of detection is to limit the energy injectionby the newly born magnetar to only a small fraction of the neutron starrotational energy, thus they should collapse soon after the merger. Our resultindicates that most supramassive neutron stars resulting from binary neutronstar mergers are short lived and they are likely to be rare in the Universe.

Constraining the long-lived supramassive neutron stars by magnetar boosted kilonovae