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The Fast Blue Optical Transient (FBOT) ATLAS18qqn (AT2018cow) has a lightcurve as bright as superluminous supernovae but rises and falls much faster. Wemodel this light curve by circumstellar interaction of a pulsationalpair-instability (PPI) supernova (SN) model based on our PPISN models studiedin previous work. We focus on the 42 $M_\odot$ He star (core of a 80$M_{\odot}$ star) which has circumstellar matter of mass 0.50 $M_\odot$. Withthe parameterized mass cut and the kinetic energy of explosion $E$, we performhydrodynamical calculations of nucleosynthesis and optical light curves ofPPISN models. The optical light curve of the first $\sim$ 20 days of AT2018cowis well-reproduced by the shock heating of circumstellar matter for the $42~M_{\odot}$ He star with $E = 5 \times 10^{51}$ erg. After day 20, the lightcurve is reproduced by the radioactive decay of 0.6 $M_\odot$ $^{56}$Co, whichis a decay product of $^{56}$Ni in the explosion. We also examine how the lightcurve shape depends on the various model parameters, such as CSM structure andcomposition. We also discuss (1) other possible energy sources and theirconstraints, (2) origin of observed high-energy radiation, and (3) how ourresult depends on the radiative transfer codes. Based on our successful modelfor AT2018cow and the model for SLSN with the CSM mass as large as $20~M_\odot)$, we propose the working hypothesis that PPISN produces SLSNe if CSMis massive enough and FBOTs if CSM is less than $\sim 1 ~M_\odot$.

A Model for Fast Blue Optical Transient AT2018Cow: Circumstellar Interaction of a Pulsational Pair-instability Supernova