SN 1054 as a Pulsar-Driven Supernova: Implications for the Crab Pulsar and Remnant Evolution

TL;DR

This paper models SN 1054 as a pulsar-driven supernova, explaining its luminosity and remnant features, and explores implications for the Crab pulsar's evolution and remnant structure.

Contribution

It introduces a pulsar-driven supernova model for SN 1054 that accounts for observed properties, offering new insights into remnant evolution and pulsar formation.

Findings

Model reproduces SN 1054 luminosity and velocity with specific pulsar parameters

Suggests pulsar spin and magnetic field influence remnant structure

Provides testable predictions through light echo observations

Abstract

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 $\sim$ 14 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.