On the Origin of the Scatter Broadening of Fast Radio Burst Pulses and Astrophysical Implications

Xu, Siyao; Zhang, Bing

doi:10.3847/0004-637x/832/2/199

Cited by 46 publications

(24 citation statements)

References 120 publications

(170 reference statements)

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“…The similar discussion is also seen in [22]. Theoretically, the broadened pulse width can be estimated as W ∼ D L θ 2 sc /2c ∼ (D L /1Gpc) × (10 10 θ sc /3) 2 × 5 ms in the context of thin screen approximation [61], where D L is luminosity distance of the source and θ sc is the corresponding scattering angle, which may account for the observed millisecond pulses of FRBs [62,63]. It indicates two important facts: 1) the observed duration of most FRBs are the upper limit of the intrinsic one and 2) the pseudo-luminosity [64] correspond to the observed duration are only the lower limit of the intrinsic luminosity.…”

Section: The Modelsupporting

confidence: 57%

Fast radio bursts from primordial black hole binaries coalescence

Deng

Cai

et al. 2018

Phys. Rev. D

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In this paper we propose the model that the coalescence of primordial black holes (PBHs) binaries with equal mass M ∼ 10 28 g can emit luminous gigahertz (GHz) radio transient, which may be candidate sources for the observed fast radio bursts (FRBs), if at least one black hole holds appropriate amount of net electric charge Q. Using a dimensionless quantity for the charge q = Q/ √ GM , our analyses infer that q ∼ O(10 −4.5 ) can explain the FRBs with released energy of order O(10 40 )ergs. With the current sample of FRBs and assuming a distribution of charge φ(q) for all PBHs, we can deduce that its form is proportional to q −3.0±0.1 for q ≥ 7.2 × 10 −5 if PBHs are sources of the observed FRBs. Furthermore, with the proposed hypothetical scenario and by estimating the local event rate of FRBs ∼ 2.6 × 10 3 Gpc −3 yr −1 , one derives a lower bound for the fraction of PBHs (at the mass of 10 28 g) against that of matter fPBH(10 28 g) 10 −5 needed to explain the rate. With this inspiring estimate, we expect that future observations of FRBs can help to falsify their physical origins from the PBH binaries coalescences. In the future, the gravitational waves produced by mergers of small black holes can be detected by high frequency gravitational wave detectors. We believe that this work would be a useful addition to the current literature on multimessenger astronomy and cosmology.

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Section: The Modelsupporting

confidence: 57%

Fast radio bursts from primordial black hole binaries coalescence

Deng

Cai

et al. 2018

Phys. Rev. D

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“…Observations show that a larger scattering tail correspond to a larger DM, e.g. τ = 2.98 × 10 −7 ms DM 1.4 (1 + 3.55 × 10 −5 DM 3.1 ) for Galactic pulsars ), a fact understandable with the turbulence theories (Xu & Zhang 2017). If one assumes that the FRBs' hosts have a similar relation, for the millisecond scattering time, one would require DM HG 280 pc cm −3 .…”

mentioning

confidence: 68%

Large Host-galaxy Dispersion Measure of Fast Radio Bursts

Yang

Luo

et al. 2017

ApJL

Self Cite

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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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“…For the host galaxy, scattering could arise in the ISM along the path (see, e.g., Cordes et al 2016;Xu & Zhang 2016) or in the immediate environs of the FRB source (see, e.g., Masui et al 2015). Because of the extremely small lever-arm factor…”

Section: Gal MCmentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,017

997

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We present a new model for the distribution of free electrons in the Galaxy, the Magellanic Clouds, and the intergalactic medium (IGM) that can be used to estimate distances to real or simulated pulsars and fast radio bursts (FRBs) based on their dispersion measure (DM). The Galactic model has an extended thick disk representing the so-called warm interstellar medium, a thin disk representing the Galactic molecular ring, spiral arms based on a recent fit to Galactic H II regions, a Galactic Center disk, and seven local features including the Gum Nebula, Galactic Loop I, and the Local Bubble. An offset of the Sun from the Galactic plane and a warp of the outer Galactic disk are included in the model. Parameters of the Galactic model are determined by fitting to 189 pulsars with independently determined distances and DMs. Simple models are used for the Magellanic Clouds and the IGM. Galactic model distances are within the uncertainty range for 86 of the 189 independently determined distances and within 20% of the nearest limit for a further 38 pulsars. We estimate that 95% of predicted Galactic pulsar distances will have a relative error of less than a factor of 0.9. The predictions of YMW16 are compared to those of the TC93 and NE2001 models showing that YMW16 performs significantly better on all measures. Timescales for pulse broadening due to interstellar scattering are estimated for (real or simulated) Galactic and Magellanic Cloud pulsars and FRBs.

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On the Origin of the Scatter Broadening of Fast Radio Burst Pulses and Astrophysical Implications

Cited by 46 publications

References 120 publications

Fast radio bursts from primordial black hole binaries coalescence

Fast radio bursts from primordial black hole binaries coalescence

Large Host-galaxy Dispersion Measure of Fast Radio Bursts

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

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