Gravitational waves within the magnetar model of superluminous supernovae and gamma-ray bursts

TL;DR

This paper investigates the role of gravitational wave emission in the energy output of magnetars powering superluminous supernovae and gamma-ray bursts, finding that GW effects are generally small unless certain parameters are large.

Contribution

It introduces constraints on GW amplitudes within the magnetar model and assesses their impact on supernova and gamma-ray burst light curves.

Findings

GW emission can significantly alter light curves if epsilon > 10^-4 or alpha > 0.01.

GW effects are more pronounced for low magnetic fields and short initial spin periods.

In most cases, GW effects are unlikely to be critical in modeling light curves due to required large amplitudes.

Abstract

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 Omega, i.e. Omega^6 (for a static 'mountain') or Omega^8 (for a r-mode fluid oscillation) versus Omega^4 for magnetic dipole radiation. Here, we use the magnetic field B and initial spin period P_0 inferred from SN and GRB observations to obtain simple constraints on the dimensionless amplitude of the mountain of epsilon < 0.01 and r-mode oscillation of alpha < 1, the former being similar to that obtained by recent works. We then include GW emission within the magnetar model. We show that when epsilon > 10^-4 (B/10^14 G) (P_0/1 ms) or alpha > 0.01 (B/10^14 G) (P_0/1 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 P_0 but are unlikely to be important in modelling SN and GRB light curves since the amplitudes needed for noticeable changes are quite large.