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The light curve of the fast radio burst (FRB) 181112 is resolved into foursuccessive pulses, and the time interval ($\sim0.8$ ms) between the first andthird pulses coincides with that between the second and fourth pulses, whichcan be interpreted as a neutron star (NS) spinning at a period of about $0.8$ms. Although this period is shorter than the most rapidly rotating pulsarcurrently known ($1.4$ ms), it is typical for a simulated massive NS formedimmediately after the coalescence of binary neutron stars (BNS). Therefore, aBNS merger is a good candidate for the origin of this FRB if the periodicity isreal. We discuss the future implications that can be obtained if such aperiodicity is detected from FRBs simultaneously with gravitational waves (GW).The remnant spin period $P_{\rm rem}$ inferred from the FRB observation isunique information which is not readily obtained by current GW observations atthe post-merger phase. If combined with the mass of the merger remnant $M_{\rmrem}$ inferred from GW data, it would set a new constraint on the equation ofstate of nuclear matter. Furthermore, the post-merger quantity $P_{\rmrem}/M_{\rm rem}$, or the tidal deformability of the merger remnant, is closelyrelated to the binary tidal deformability parameter $\Lambda$ of NSs beforethey merge, and a joint FRB-GW observation will establish a new limit on$\Lambda$. Thus, if $\Lambda$ is also well measured by GW data, a comparisonbetween these two will provide further insights into the nature of nuclearmatter and BNS mergers.

FRB 181112 as a Rapidly-Rotating Massive Neutron Star just after a  Binary Neutron Star Merger?: Implications for Future Constraints on Neutron  Star Equations of State