Supergiant Pulses from Extragalactic Neutron Stars

TL;DR

This paper investigates the physical mechanisms, detectability, and rates of supergiant radio pulses from extragalactic neutron stars, proposing models that align with observed burst rates and energies, and discussing observational signatures.

Contribution

It introduces a detailed physical model for supergiant pulses from extragalactic neutron stars, linking burst properties to emission physics and detection limits.

Findings

Burst rates match neutron star formation rates in a Hubble volume.

Single shot pulses resemble Crab pulsar's extreme pulses.

Detection distance limited to a few hundred Mpc for typical energies.

Abstract

We consider radio bursts that originate from extragalactic neutron stars (NSs) by addressing three questions about source distances. What are the physical limitations on coherent radiation at GHz frequencies? Do they permit detection at cosmological distances? How many bursts per NS are needed to produce the inferred burst rate $\sim 10^3$-$10^4 $sky$^{-1}$ day$^{-1}$? The burst rate is comparable to the NS formation rate in a Hubble volume, requiring only one per NS if they are bright enough. However, radiation physics causes us to favor a closer population. More bursts per NS are then required but repeats in 10 to 100 yr could still be negligible. Bursts are modeled as sub-ns, coherent shot pulses superposed incoherently to produce ms-duration $\sim 1$ Jy amplitudes; each shot-pulse can be much weaker than the burst amplitude, placing less restrictive requirements on the emission process. Nonetheless, single shot pulses are similar to the extreme, unresolved ($< 0.4$ ns) MJy shot pulse seen from the Crab pulsar, which is consistent with coherent curvature radiation emitted near the light cylinder by an almost neutral clump with net charge $\sim \pm 10^{21}e$ and total energy $\gtrsim 10^{23}$ ergs. Bursts from Gpc distances require incoherent superposition of $\sim 10^{12}d_{\rm Gpc}^2$ shot pulses or a total energy $\gtrsim 10^{35} d_{\rm Gpc}^2$ erg. The energy reservoir near the light cylinder limits the detection distance to $\lesssim {\rm few} \times 100$ Mpc for a fluence $\sim 1$ Jy ms unless conditions are more extreme than for the Crab pulsar. Similarly, extreme single pulses from ordinary pulsars and magnetars could be detectable from throughout the Local Group and perhaps farther. Contributions to dispersion measures from galaxy clusters will be significant for some of the bursts. We discuss tests for the signatures of bursts associated with extragalactic NSs.