Fast radio bursts — A brief review: Some questions, fewer answers

Katz, J. I.

doi:10.1142/s0217732316300135

Cited by 126 publications

(129 citation statements)

References 56 publications

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“…(11) and (12), we can then integrate the resulting ∆ρ E ≡ ρ l=1 E − ρ l=0 E over the bubble region to yield a total released energy of ≈ 4 × 10 39 B 2 11 ergs. This result appears to be in good agreement with the implied energy of 10 38 − 10 40 ergs for the FRBs (Katz (2016a)), noting that these observation-implied numbers may be slight overestimates, however, depending on which fraction of the DMs is appropriated into the intergalactic medium (see Sect. 7 below).…”

Section: Bubble-free Magnetospheresupporting

confidence: 85%

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Pulsar magnetospheric convulsions induced by an external magnetic field

Zhang

2017

A&A

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The canonical pulsar magnetosphere contains a bubble of closed magnetic field lines that is separated from the open lines by current sheets, and different branches of such sheets intersect at a critical line on the light cylinder (LC). The LC is located far away from the neutron star, and the pulsar's intrinsic magnetic field at that location is much weaker than the commonly quoted numbers applicable to the star surface. The magnetic field surrounding supermassive black holes that reside in galactic nuclei is of comparable or greater strength. Therefore, when the pulsar travels inside such regions, a non-negligible Lorentz force is experienced by the current sheets, which tends to pull them apart at the critical line. As breakage occurs, instabilities ensue that burst the bubble, allowing closed field lines to snap open and release large amounts of electromagnetic energy, sufficient to power fast radio bursts (FRBs). This process is necessarily associated with an environment of a strong magnetic field and thus might explain the large rotation measures recorded for the FRBs. We sketch a portrait of the process and examine its compatibility with several other salient features of the FRBs.

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Section: Bubble-free Magnetospheresupporting

confidence: 85%

“…The enormous distance scales that come with this assumption imply that a large amount of energy needs to be available, 10 38 −10 40 ergs, to be more precise (Katz (2016a), assuming isotropic emission). In addition, the short pulse duration requires a compact source region.…”

Section: Introductionmentioning

confidence: 99%

Pulsar magnetospheric convulsions induced by an external magnetic field

Zhang

2017

A&A

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“…The catastrophic models (e.g., Totani 2013; Kashiyama et al 2013;Falcke & Rezzolla 2014;Zhang 2014Zhang , 2016aWang et al 2016) cannot interpret the repeating FRB 121102. The previously favored super-giant-pulse model (in analogy to nanoshots from the Crab pulsar; Cordes & Wasserman 2016;Connor et al 2016) invokes nearby galaxy not at the cosmological distances and therefore are challenged by the fact that the repeater is located in a host galaxy at redshift z=0.193 (Tendulkar et al 2017; but see Katz 2016aKatz , 2016b. The magnetar giant flare model (Popov & Postnov 2010;Kulkarni et al 2014;Katz 2016c) is in apparent conflict with the non-detection of bright radio pulse from the SGR 1806-20 giant flare (Tendulkar et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A “Cosmic Comb” Model of Fast Radio Bursts

Zhang

2017

ApJL

163

144

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Recent observations of fast radio bursts (FRBs) indicate a perplexing, inconsistent picture. We propose a unified scenario to interpret diverse FRBs observed. A regular pulsar, otherwise unnoticeable at a cosmological distance, may produce a bright FRB if its magnetosphere is suddenly "combed" by a nearby, strong plasma stream toward the anti-stream direction. If the Earth is to the night side of the stream, the combed magnetic sheath would sweep across the direction of Earth and make a detectable FRB. The stream could be an AGN flare, a GRB or supernova blastwave, a tidal disruption event, or even a stellar flare. Since it is the energy flux received by the pulsar rather than the luminosity of the stream origin that defines the properties of the FRB, this model predicts a variety of counterparts of FRBs, including a possible connection between FRB 150418 and an AGN flare, a possible connection between FRB 131104 and a weak GRB, a steady radio nebula associated with the repeating FRB 121102, and probably no bright counterparts for some FRBs.

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“…Catastrophic event models are able to explain non-repeating burst , including the merger of compact objects (Kashiyama et al 2013;Wang et al 2016), super massive neutron stars collapsing to black holes (Falcke & Rezzolla 2014;Zhang 2014), and so on. The repeating burst is more likely to originate from young remnants of stellar collapses, neutron stars or black holes (Katz 2016a), e.g. soft gamma repeaters (Pen & Connor 2015;Katz 2016c), giant pulse from young pulsars (Keane et al 2012;Katz 2016b), and the interaction of pulsars with planets (Mottez & Zarka 2014), asteroids or comets (Geng & Huang 2015;Dai et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A Fast Radio Burst Search Method for VLBI Observation

Liu¹,

Tong²,

Zheng³

et al. 2018

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We introduce the cross spectrum based FRB (Fast Radio Burst) search method for VLBI observation. This method optimizes the fringe fitting scheme in geodetic VLBI data post processing, which fully utilizes the cross spectrum fringe phase information and therefore maximizes the power of single pulse signals. Working with cross spectrum greatly reduces the effect of radio frequency interference (RFI) compared with using auto spectrum. Single pulse detection confidence increases by cross identifying detections from multiple baselines. By combining the power of multiple baselines, we may improve the detection sensitivity. Our method is similar to that of coherent beam forming, but without the computational expense to form a great number of beams to cover the whole field of view of our telescopes. The data processing pipeline designed for this method is easy to implement and parallelize, which can be deployed in various kinds of VLBI observations. In particular, we point out that VGOS observations are very suitable for FRB search.

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Fast radio bursts — A brief review: Some questions, fewer answers

Cited by 126 publications

References 56 publications

Pulsar magnetospheric convulsions induced by an external magnetic field

Pulsar magnetospheric convulsions induced by an external magnetic field

A “Cosmic Comb” Model of Fast Radio Bursts

A Fast Radio Burst Search Method for VLBI Observation

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