Discovery of millisecond radio bursts from M 87

Linscott, I. R.; Erkes, J. W.

doi:10.1086/183209

Cited by 28 publications

(24 citation statements)

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“…Then, most observed FRBs ought to have energies near the peak of the distributions. We display the approximate 5 energies of FRBs with possible localizations (see Linscott & Erkes 1980;Tendulkar et al 2017;Bannister et al 2019;Ravi et al 2019) in Figure 2 -it is apparent that the theoretical narrowness is largely consistent with the inferred FRB energies, except perhaps for case α = 1. Notably, although the "normal" and "extended" birth B 0 ranges do shift the distributions, the value of α clearly has the greatest impact on the shape and width of these FRB luminosity functions.…”

Section: Energy/luminosity Functionsupporting

confidence: 56%

“…• The population energy/luminosity function is somewhat narrow, with FWHM of 1 − 3 decades with a sharp low-energy cut-off around 10 37 − 10 38 erg. The narrowness implies high probability of observing FRB energy corresponding to the peak of the luminosity function, and lends credence to the radio bursts detected by Linscott & Erkes (1980) as originating from Virgo. Moreover, the narrowness suggests redshifts may be constrained solely by FRB fluence once the luminosity function is better characterized.…”

Section: Summary and Discussionmentioning

confidence: 64%

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The Fast Radio Burst Luminosity Function and Death Line in the Low-twist Magnetar Model

Wadiasingh

Beniamini

Timokhin

et al. 2020

ApJ

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We explore the burst energy distribution of fast radio bursts (FRBs) in the low-twist magnetar model of Wadiasingh & Timokhin (2019). Motivated by the power-law fluence distributions of FRB 121102, we propose an elementary model for the FRB luminosity function of individual repeaters with an inversion protocol which directly relates the power-law distribution index of magnetar short burst fluences to that for FRBs. The protocol indicates the FRB energy scales virtually linearly with crust/field dislocation amplitude, if magnetar short bursts prevail in the magnetoelastic regime. Charge starvation in the magnetosphere during bursts (required in WT19) for individual repeaters implies the predicted burst fluence distribution is narrow, < ∼ 3 decades for yielding strains and oscillation frequencies feasible in magnetar crusts. Requiring magnetic confinement and charge starvation, we obtain a death line for FRBs which segregates magnetars from the normal pulsar population, suggesting only the former will host FRBs. We convolve the burst energy distribution for individual magnetars to define the distribution of luminosities in evolved magnetar populations. The broken power-law luminosity function's low energy character depends on the population model, while the high energy index traces that of individual repeaters. Independent of the evolved population, the broken power-law isotropic-equivalent energy/luminosity function peaks at ∼ 10 38 − 10 40 erg with a sharp low-energy cutoff at < ∼ 10 37 erg. Lastly, we consider the local fluence distribution of FRBs, and find that it can constrain the subset of FRB-producing magnetar progenitors. Our model suggests that improvements in sensitivity may reveal flattening of the global FRB fluence distribution and saturation in FRB rates. 1/7 c and ε CR,pp ∝ ρ 1/2 c . There also exist regimes between B ∼ 10 13 − 10 14 G where the splitting length may be shorter than the pair length, owing to the dependence of splitting amplitude integrals M σ on B (for details, see Hu et al. 2019). A more complete study of pair cascades with splitting for FRB models is deferred to the future.

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Section: Energy/luminosity Functionsupporting

confidence: 56%

Section: Summary and Discussionmentioning

confidence: 64%

The Fast Radio Burst Luminosity Function and Death Line in the Low-twist Magnetar Model

Wadiasingh

Beniamini

Timokhin

et al. 2020

ApJ

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“…The discovery of FRBs as an observational class has also prompted re-examination of previously published transients surveys such as the reported discovery of highly dispersed radio pulses from M87 in the Virgo cluster in 1980 (Linscott and Erkes, 1980) and the 1989 sky survey with the Molonglo Observatory Synthesis Telescope by Amy et al (1989), which discovered an excess of non-terrestrial short-duration bursts (1 µs to 1 ms) in 4000 hours of observations. These unexplained bursts showed no clustering in time or position and were not associated with known Galactic sources.…”

Section: A Brief Historymentioning

confidence: 99%

Fast radio bursts

Petroff

Hessels

Lorimer

2019

Astron Astrophys Rev

622

471

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The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar to the individual pulses from pulsars, their large dispersive delays suggest that they originate from far outside the Milky Way and hence are many ordersof-magnitude more luminous. While most FRBs appear to be one-off, perhaps cataclysmic events, two sources are now known to repeat and thus clearly have a longer-lived central engine. Beyond understanding how they are created, there is also the prospect of using FRBs -as with pulsars -to probe the extremes of the Universe as well as the otherwise invisible intervening medium. Such studies will be aided by the high implied all-sky event rate: there is a detectable FRB roughly once every minute occurring somewhere on the sky. The fact that less than a hundred FRB sources have been discovered in the last decade is largely due to the small fields-of-view of current radio telescopes. A new generation of wide-field instruments is now coming online, however, and these will be capable of detecting multiple FRBs per day. We are thus on the brink of further breakthroughs in the short-duration radio transient phase space, which will be critical for differentiating between the many proposed theories for the origin of FRBs. In this review, we give an observational and theoretical introduction at a level that is accessible to astronomers entering the field.

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“…Particular galaxies were searched for several hours without detection of giant pulses (e.g., Osullivan et al 1978;Cordes & McLaughlin 2003). Linscott & Erkes (1980) report pulses from M87 having a DM between 1000 and 6000 cm −3 pc, but Hankins et al (1981) were not able to confirm them. Rubio-Herrera et al (2013) published possible candidates from M31 having a DM of 54.7 cm −3 pc.…”

Section: Introductionmentioning

confidence: 99%

Short-Duration Radio Bursts With Apparent Extragalactic Dispersion

Saint-Hilaire

Benz

Monstein

2014

ApJ

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We present the results of the longest yet undertaken search for apparently extragalactic radio bursts at the Bleien Radio Observatory covering 21,000 hr (898 days). The data were searched for events of less than 50 ms FWHM duration showing a ν −2 drift in the spectrogram characteristic of the delay of radio waves in plasma. We have found five cases suggesting dispersion measures between 350 and 400 cm −3 pc while searching in the range of 75-2000 cm −3 pc. Four of the five events occurred between 10:27 and 11:24 a.m. local civil time. The only exception occurred at night with the full Moon in the beam. It was an event that poorly fits plasma dispersion, but had the characteristics of a solar Type III burst. However, we were not able to confirm that it was a lunar reflection. All events were observed with a log-periodic dipole within 6800 hr, but none with a more directional horn antenna observing the rest of the time. These properties suggest a terrestrial origin of the "peryton" type reported before. However, the cause of these events remains ambiguous.

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Discovery of millisecond radio bursts from M 87

Cited by 28 publications

References 0 publications

The Fast Radio Burst Luminosity Function and Death Line in the Low-twist Magnetar Model

The Fast Radio Burst Luminosity Function and Death Line in the Low-twist Magnetar Model

Fast radio bursts

Short-Duration Radio Bursts With Apparent Extragalactic Dispersion

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