2016MNRAS.463..489H

The light curve of many supernovae (SNe) and gamma-ray bursts (GRBs) can be explained by a sustained injection of extra energy from its possible central engine, a rapidly rotating strongly magnetic neutron star (i.e. magnetar). The magnetic dipole radiation power that the magnetar supplies comes at the expense of the star's rotational energy. However, radiation by gravitational waves (GWs) can be more efficient than magnetic dipole radiation because of its stronger dependence on neutron star spin rate Ω, i.e. Ω⁶ (for a static 'mountain') or Ω⁸ (for an r-mode fluid oscillation) versus Ω⁴ for magnetic dipole radiation. Here, we use the magnetic field B and initial spin period P₀ inferred from SN and GRB observations to obtain simple constraints on the dimensionless amplitude of the mountain of ε < 0.01 and r-mode oscillation of α < 1, the former being similar to that obtained by recent works. We then include GW emission within the magnetar model. We show that when ε > 10^–4(B/10¹⁴ G)(P₀/1 ms) or α > 0.01(B/10¹⁴ G)(P₀/1 ms)², light curves are strongly affected, with significant decrease in peak luminosity and increase in time to peak luminosity. Thus, the GW effects studied here are more pronounced for low B and short P₀ but are unlikely to be important in modelling SN and GRB light curves since the amplitudes needed for noticeable changes are quite large.