Gamma-ray bursts from extragalactic Magnetar Flares

The prototype for events that we call MFs—“March Fifth” events or “Magnetar Flares”—was observed on March 5, 1979. There is evidence that MFs are powered by catastrophic magnetic instabilities in ultra-magnetized neutron stars. These events begin with brief $(Δt∼0.1–1 s),$ intense, hard spikes of gamma rays, probably emitted in concurrence with relativistic outflows; followed by long $(t∼100 s)$ softer tails of hard X-rays, modulated on the stellar rotation period. Prototypical MFs could have been detected by BATSE out to ∼13 Mpc, nearly reaching the Virgo cluster. The likely number of isotropic, standard-candle MFs detected by the BATSE experiment is ∼12. These short-duration, fast-rising gamma-ray bursts could in principle be identified by their positional coincidences with nearby galaxies and the Supergalactic Plane. The ensuing soft tail emission would not have been detected by BATSE for sources more distant than the Andromeda Galaxy. Bayes’ Theorem implies that there is a ∼99% chance for at least 1 isotropic MF in the BATSE catalog, and a ∼16% chance for more than 20. It is possible that MFs also emit an intense, hard, beamed component during the initial spike phase. If this beamed component has opening angle $ψ=8°ψ8$ and peak luminosity comparable to the power of the isotropic component, then BATSE would detect such beamed sources out to redshift $z∼0.1ψ8−1,$ at a full-sky rate of $ṄB∼100ψ8−1 yr−1.$ We speculate that such beamed MFs could account for the short, hard Class II gamma-ray bursts (GRBs) in the BATSE catalog, or some significant subset of them. If true, then Class II GRBs positions should correlate with the positions of galaxies and galaxy clusters within ∼350 Mpc.