How Much Can $^{56}$Ni Be Synthesized by Magnetar Model for Long Gamma-ray Bursts and Hypernovae?

TL;DR

This paper investigates the potential of magnetar models to produce sufficient $^{56}$Ni for bright hypernovae by analyzing shock wave evolution and deriving constraints on magnetar parameters.

Contribution

It provides a quantitative estimate of the magnetar magnetic field and rotation rate needed to synthesize enough $^{56}$Ni for hypernova brightness.

Findings

Derived a constraint on magnetar parameters for $^{56}$Ni synthesis.

Estimated the temperature evolution of shock waves driven by magnetar winds.

Linked magnetar properties to observable hypernova brightness.

Abstract

A rapidly rotating neutron star with strong magnetic fields, called magnetar, is a possible candidate for the central engine of long gamma-ray bursts and hypernovae (HNe). We solve the evolution of a shock wave driven by the wind from magnetar and evaluate the temperature evolution, by which we estimate the amount of $^{56}$Ni that produces a bright emission of HNe. We obtain a constraint on the magnetar parameters, namely the poloidal magnetic field strength ($B_p$) and initial angular velocity ($\Omega_i$), for synthesizing enough $^{56}$Ni mass to explain HNe ($M_{^{56}\mathrm{Ni}}\gtrsim 0.2M_\odot$), i.e. $(B_p/10^{16}~\mathrm{G})^{1/2}(\Omega_i/10^4~\mathrm{rad~s}^{-1})\gtrsim 0.7$.