Bright Supernovae from Magnetar Birth

TL;DR

This paper explores how magnetar-powered mechanisms can produce extremely luminous supernovae, emphasizing the role of magnetic fields and initial explosion energy in shaping their light curves.

Contribution

It introduces a model where magnetar dipole radiation significantly influences supernova brightness, independent of nickel mass, and discusses resulting light curve features.

Findings

Peak luminosity depends on magnetar magnetic field strength.

Tail of light curve can surpass radioactive decay luminosity.

High initial energies lead to higher velocities and brightness.

Abstract

Following an initial explosion that might be launched either by magnetic interactions or neutrinos, a rotating magnetar radiating according to the classic dipole formula could power a very luminous supernova. While some 56Ni might be produced in the initial explosion, the peak of the light curve in a Type I supernova would not be directly related to its mass. In fact, the peak luminosity would be most sensitive to the dipole field strength of the magnetar. The tail of the light curve could resemble radioactive decay for some time but, assuming complete trapping of the pulsar emission, would eventually be brighter. Depending on the initial explosion energy, both high and moderate velocities could accompany a very luminous light curve.