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We investigate effects of energetic pulsar wind nebulae (PWNe) on dust formation and evolution. Dust emission has been observed in many supernova remnants that also have neutron stars as compact remnants. We study the dependence of dust formation time and size on properties of the ejecta and central pulsar. We find that a pulsar with an initial spin period |$P \sim 1\hbox{-}10\, \rm ms$| and a dipole magnetic field |$B \sim 10^{12\hbox{-}15}\, \rm G$| can either accelerate or delay dust formation, with a time-scale of several months to over 10 yr, and reduce the average size of dust by a factor of ∼10 or more compared to the non-pulsar case. We also find that infrared dust emission may be detectable in typical superluminous supernovae out to ∼100–1000 Mpc in 2–5 yr after the explosion, although this depends sensitively on the spectral index of non-thermal emission from the nebula. We discuss implications to previous supernova observations. Some discrepancies between dust formation models and observations, such as the formation time in SN1987A or the dust size in the Crab Nebula, could be explained by the influence of a pulsar, and knowledge of the dust emission will be important for future ALMA observations of superluminous supernovae. [ABSTRACT FROM AUTHOR]

It has been widely argued that Type-I superluminous supernovae (SLSNe-I) are driven by powerful central engines with a long-lasting energy injection after the core-collapse of massive progenitors. One of the popular hypotheses is that the hidden engines are fast-rotating pulsars with amagnetic field of B~1013-1015 G. Murase, Kashiyama & Mészáros proposed that quasisteady radio/submm emission from non-thermal electron-positron pairs in nascent pulsar wind nebulae can be used as a relevant counterpart of such pulsar-driven supernovae (SNe). In this work, focusing on the nascent SLSN-I remnants, we examine constraints that can be placed by radio emission. We show that the Atacama Large Millimeter/submillimetre Array can detect the radio nebula from SNe at DL ~ 1 Gpc in a few years after the explosion, while the Jansky Very Large Array can also detect the counterpart in a few decades. The proposed radio follow-up observation could solve the parameter degeneracy in the pulsar-driven SN model for optical/UV light curves, and could also give us clues to young neutron star scenarios for SLSNe-I and fast radio bursts. [ABSTRACT FROM AUTHOR]