Fast Radio Bursts From the Inspiral of Double Neutron Stars

Wang, Jie-Shuang; Yang, Yuan-Pei; Wu, Xue-Feng; Dai, Z. G.; Wang, F. Y.

doi:10.3847/2041-8205/822/1/l7

Cited by 200 publications

(160 citation statements)

References 47 publications

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“…Some other models have specific predictions that can be tested by future observations. For example, if future localizations of FRBs all reveal associations with bright radio nebulae, it would suggest a newborn millisecond magnetar as the source of FRBs (e.g., Murase et al 2016;Metzger et al 2017), an FRB coincident with a gravitational-wave (GW) signal due to an NS-NS, NS-BH, or black hole-black hole merger would suggest a direct connection between the FRB and the merger (Totani 2013;Zhang 2016a;Wang et al 2016) 3 ; and an FRB coincident with the disappearance of an extended plateau emission would suggest the ejection of a magnetosphere during the collapse of a supramassive neutron star ("blitzar") as the mechanism of FRBs (Zhang 2014;Falcke & Rezzolla 2014).…”

Section: Discussionmentioning

confidence: 99%

“…A radio afterglow was not detected (Shannon & Ravi 2016), but the non-detection is consistent with the afterglow model if the ambient density is low (as expected from the neutron star-neutron star (NS-NS) or neutron star-black hole (NS-BH) merger models) or the shock microphysics parameters are low (Murase et al 2017;Gao & Zhang 2017;Dai et al 2016a). The possible mechanisms that might produce an FRB associated with a GRB include collapse of a supramassive millisecond magnetar to a black hole (Zhang 2014), which requires that the FRB appears near the end of an extended X-ray plateau, or premerger electromagnetic processes (Zhang 2016a(Zhang , 2016bWang et al 2016), which require that the FRB leads the burst. The latter scenario may be argued to marginally match the data (Dai et al 2016a;Gao & Zhang 2017).…”

Section: Case Studiesmentioning

confidence: 99%

“…However, no model can explain all the above observational facts. 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.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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Section: Discussionmentioning

confidence: 99%

Section: Case Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A “Cosmic Comb” Model of Fast Radio Bursts

Zhang

2017

ApJL

163

144

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“…For the models invoking compact object mergers (e.g. Totani 2013;Wang et al 2016), the contribution from a near-source plasma may not be important (except for "prompted" mergers that have a short time delay from star formation). Some of these systems may also have a large offset from the host galaxy, which may not give a large local DM.…”

Section: Discussionmentioning

confidence: 99%

Large Host-galaxy Dispersion Measure of Fast Radio Bursts

Yang

Luo

et al. 2017

ApJL

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Fast radio bursts (FRBs) have excessive dispersion measures (DMs) and an all-sky distribution, which point toward an extragalactic or even a cosmological origin. We develop a method to extract the mean host galaxy DM ( DM HG,loc ) and the characterized luminosity (L) of FRBs using the observed DM-Flux data, based on the assumption of a narrow luminosity distribution. Applying Bayesian inference to the data of 21 FRBs, we derive a relatively large mean host DM, i.e. DM HG,loc ∼ 270 pc cm −3 with a large dispersion. A relatively large DM HG of FRBs is also supported by the millisecond scattering times of some FRBs and the relatively small redshift z = 0.19273 of FRB 121102 (which gives DM HG,loc ∼ 210 pc cm −3 ). The large host galaxy DM may be contributed by the ISM or a near-source plasma in the host galaxy. If it is contributed by the ISM, the type of the FRB host galaxies would not be Milky Way (MW)-like, consistent with the detected host of FRB 121102. We also discuss the possibility of having a near-source supernova remnant (SNR), pulsar wind nebula (PWN) or HII region that gives a significant contribution to the observed DM HG .

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“…A claimed association of FRB150418 with a centimeter-wavelength afterglow and host galaxy (Keane et al 2016) has been disputed and instead attributed to common AGN variability, either intrinsic (Vedantham et al 2017;Williams & Berger 2016) or caused by Milky Way scintillation (Akiyama & Johnson 2016;Johnston et al 2016). With so little detail on the locations of FRBs, theories for their production and sources are understandably varied, ranging from ultabright pulses from pulsars (Cordes & Wasserman 2016), flares from magnetars (Lyubarsky 2014;Katz 2016), binary neutron star mergers (Wang et al 2016), or cosmic strings (Cai et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Radio-interferometric Monitoring of FRB 131104: A Coincident AGN Flare, but No Evidence for a Cosmic Fireball

Shannon

Ravi

2017

ApJL

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The localization of fast radio bursts (FRBs) has been hindered by the poor angular resolution of the detection observations and inconclusive identification of transient or variable counterparts. Recently a γ-ray pulse of 380 s duration has been associated with FRB 131104. We report on radio-continuum imaging observations of the original localization region of the FRB, beginning three days after the event and comprising 25 epochs over 2.5 years. We argue that the probability of an association between the FRB and the γ-ray transient has been overestimated. We provide upper limits on radio afterglow emission that would be predicted if the γ-ray transient was associated with an energetic γ-ray burst. We further report the discovery of an unusual variable radio source spatially and temporally coincident with FRB131104, but not spatially coincident with the γ-ray event. The radio variable flares by a factor of 3 above its long-term average within 10 day of the FRB at 7.5 GHz, with a factor-of-2 increase at 5.5 GHz. Since the flare, the variable has persisted with only modest modulation and never approached the flux density observed in the days after the FRB. We identify an optical counterpart to the variable. Optical and infrared photometry, and deep optical spectroscopy, suggest that the object is a narrow-line radio active galactic nucleus.

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Fast Radio Bursts From the Inspiral of Double Neutron Stars

Cited by 200 publications

References 47 publications

A “Cosmic Comb” Model of Fast Radio Bursts

A “Cosmic Comb” Model of Fast Radio Bursts

Large Host-galaxy Dispersion Measure of Fast Radio Bursts

Radio-interferometric Monitoring of FRB 131104: A Coincident AGN Flare, but No Evidence for a Cosmic Fireball

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