Burst timescales and luminosities link young pulsars and fast radio bursts

Nimmo, K.; Hessels, J. W. T.; Kirsten, F.; Keimpema, A.; Cordes, J. M.; Snelders, M. P.; Hewitt, D. M.; Karuppusamy, R.; Archibald, Anne M.; Bezukovs, V.

doi:10.48550/arxiv.2105.11446

Cited by 38 publications

(63 citation statements)

References 80 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Such broadband frequency modulations are observed in FRBs (e.g. Shannon et al 2018;Hessels et al 2019;Nimmo et al 2021). The bandwidth increases with the burst frequency (Eqs.…”

Section: Warm Magnetar Windmentioning

confidence: 91%

See 1 more Smart Citation

Filamentation of Fast Radio Bursts in magnetar winds

Sobacchi,

Lyubarsky,

Beloborodov

et al. 2021

Preprint

View full text Add to dashboard Cite

Magnetars are the most promising progenitors of Fast Radio Bursts (FRBs). Strong FRB radio waves propagating through the magnetar wind are subject to non-linear effects, including modulation/filamentation instabilities. In pair plasmas, spatial modulations of the wave intensity grow exponentially because the ponderomotive force pushes particles outside regions of enhanced radiation intensity. Then in these regions the plasma refractive index increases, which creates a converging lens that further enhances the radiation intensity. Since in magnetically-dominated plasmas the ponderomotive force pushes particles primarily along the field lines, the FRB radiation intensity develops sheets perpendicular to the direction of the wind magnetic field. The radiation sheets are eventually scattered due to diffraction. The FRB scattering timescale depends on the properties of the magnetar wind. In a cold wind, the typical scattering timescale is τ sc ∼ µs − ms at the frequency ν ∼ 1 GHz. The scattering timescale increases at low frequencies, with the scaling τ sc ∝ ν −2 . The frequency-dependent broadening of the brightest pulse of FRB 181112 is consistent with this scaling. From the scattering timescale of the pulse, one can estimate that the wind Lorentz factor is larger than a few tens. In a warm wind, the scattering timescale can approach τ sc ∼ ns. Then scattering produces a frequency modulation of the observed intensity with a large bandwidth, ∆ν ∼ 1/τ sc 100 MHz. Broadband frequency modulations observed in FRBs could be due to scattering in a warm magnetar wind.

show abstract

“…Such broadband frequency modulations are observed in FRBs (e.g. Shannon et al 2018;Hessels et al 2019;Nimmo et al 2021). The bandwidth increases with the burst frequency (Eqs.…”

Section: Warm Magnetar Windmentioning

confidence: 91%

“…Broadband frequency modulations observed in FRBs (e.g. Shannon et al 2018;Hessels et al 2019;Nimmo et al 2021) could be due to scattering in a warm magnetar wind.…”

Section: Scattering Of Fast Radio Burstsmentioning

confidence: 99%

Filamentation of Fast Radio Bursts in magnetar winds

Sobacchi,

Lyubarsky,

Beloborodov

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…However, arguably the strongest evidence for an FRB-magnetar link arises from the detection of FRB-like bursts from the Galactic magnetar SGR 1935+2154(CHIME/FRB Collaboration et al 2020;Bochenek et al 2020;Kirsten et al 2021). These Galactic bursts had similar signatures and durations to extragalactic FRBs, however, when compared the subset of extragalactic FRBs which have been localised to host galaxies, they appear much less luminous (e.g., Nimmo et al 2021). The luminosity of the SGR 1935+2154 bursts means that they would not be detectable in external galaxies, and so the lack of similar luminosity bursts in the extragalactic sample is not surprising.…”

Section: Introductionmentioning

confidence: 92%

The Fast Radio Burst-emitting magnetar SGR 1935+2154 -- proper motion and variability from long-term Hubble Space Telescope monitoring

Lyman,

Levan,

Wiersema

et al. 2021

Preprint

View full text Add to dashboard Cite

We present deep Hubble Space Telescope near-infrared (NIR) observations of the magnetar SGR 1935+2154 from June 2021, approximately 6 years after the first HST observations, a year after the discovery of fast radio burst like emission from the source, and in a period of exceptional high frequency activity. Although not directly taken during a bursting period the counterpart is a factor of ∼ 1.5 to 2.5 brighter than seen at previous epochs with F140W(AB) = 24.65 ± 0.02 mag. We do not detect significant variations of the NIR counterpart within the course of any one orbit (i.e. on minutes-hour timescales), and contemporaneous X-ray observations show SGR 1935+2154 to be at the quiescent level. With a time baseline of 6 years from the first identification of the counterpart we place stringent limits on the proper motion of the source, with a measured proper motion of µ = 3.1 ± 1.5 mas yr −1 . The direction of proper motion indicates an origin of SGR 1935+2154 very close to the geometric centre of SNR G57.2+08, further strengthening their association. At an adopted distance of 6.6 ± 0.7 kpc, the corresponding tangential space velocity is ν T = 97 ± 48 km s −1 (corrected for differential Galactic rotation and peculiar Solar motion), although its formal statistical determination may be compromised owing to few epochs of observation. The current velocity estimate places it at the low end of the kick distribution for pulsars, and makes it among the lowest known magnetar kicks. When collating the few-magnetar kick constraints available, we find full consistency between the magnetar kick distribution and the much larger pulsar kick sample.

show abstract

“…Bursts with T B ≥ T B,cri are considered as "classical" FRBs. Since this critical value is unknown, tentatively we choose T B,cri = 10 33 K indicated by the plot of spectral luminosity-duration phase space (Keane 2018;Nimmo et al 2021;Petroff et al 2021). The influence of choosing different T B,cri will be discussed later in Section 3.…”

Section: Frb Classification By Brightness Temperaturementioning

confidence: 99%

“…They cluster in different regions of the spectral luminosity-duration phase space for radio transients, and the most prominent difference between them is T B (e.g., Fig. 3 of Nimmo et al 2021). However, the critical value T B,cri to define an FRB is not well known.…”

Section: Introductionmentioning

confidence: 99%

New Insights into the Criteria of Fast Radio Burst in the Light of FRB 20121102A

Xiao,

Dai

2021

Preprint

View full text Add to dashboard Cite

The total event number of fast radio bursts (FRBs) is accumulating rapidly with the improvement of existing radio telescopes and the completion of new facilities. Especially, the Five-hundred-meter Aperture Spherical radio Telescope (FAST) Collaboration has just reported more than one thousand bursts in a short observing period of 47 days (Li et al. 2021). The interesting bimodal distribution in their work motivates us to revisit the definition of FRBs. In this work, we ascribe the bimodal distribution to two physical kinds of radio bursts, which may have different radiation mechanisms. We propose to use brightness temperature to separate two subtypes. For FRB 20121102A, the critical brightness temperature is T B,cri ≃ 10 33 K. Bursts with T B ≥ T B,cri are denoted as "classical" FRBs, and further we find a tight pulse width-fluence relation (T ∝ F ν 0.306 ) for them. On the contrary, the other bursts are considered as "atypical" bursts that may originate from a different physical process. We suggest that for each FRB event, a similar dividing line should exist but T B,cri is not necessarily the same. Its exact value depends on FRB radiation mechanism and properties of the source.

show abstract

Burst timescales and luminosities link young pulsars and fast radio bursts

Cited by 38 publications

References 80 publications

Filamentation of Fast Radio Bursts in magnetar winds

Filamentation of Fast Radio Bursts in magnetar winds

The Fast Radio Burst-emitting magnetar SGR 1935+2154 -- proper motion and variability from long-term Hubble Space Telescope monitoring

New Insights into the Criteria of Fast Radio Burst in the Light of FRB 20121102A

Contact Info

Product

Resources

About