  One of the most studied objects in astronomy, the Crab Nebula, is the remnant
of the historical supernova SN 1054. Historical observations of the supernova
imply a typical supernova luminosity, but contemporary observations of the
remnant imply a low explosion energy and low ejecta kinetic energy. These
observations are incompatible with a standard $^{56}$Ni-powered supernova,
hinting at an an alternate power source such as circumstellar interaction or a
central engine. We examine SN 1054 using a pulsar-driven supernova model,
similar to those used for superluminous supernovae. The model can reproduce the
luminosity and velocity of SN 1054 for an initial spin period of $\sim$ 13 ms
and an initial dipole magnetic field of 10$^{14-15}$ G. We discuss the
implications of these results, including the evolution of the Crab pulsar, the
evolution of the remnant structure, formation of filaments, and limits on
freely expanding ejecta. We discuss how our model could be tested further
through potential light echo photometry and spectroscopy, as well as the modern
analogues of SN 1054.
