FRB 200428: an Impact between an Asteroid and a Magnetar

Geng, Jin-Jun; Li, Bing; Li, Long-Biao; Xiong, Shao-Lin; Kuiper, Rolf; Huang, Yong-Feng

doi:10.48550/arxiv.2006.04601

Cited by 3 publications

(3 citation statements)

References 50 publications

(57 reference statements)

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“…Many models have been proposed to explain the high brightness temperate of FRBs, which usually involve magnetized compact stars as progenitors, especially neutron stars (NS) (see Platts et al 2018, for a rencent review). In particular, it is widely suggested that young flaring magnetars (Popov & Postnov (2013); Lyubarsky (2014); Waxman (2017); Beloborodov (2017); Lu & Kumar (2018); Yang & Zhang (2018); Margalit & Metzger (2018); Katz (2018); Beloborodov (2019); Metzger et al (2019); ; Margalit et al (2020); Wang & Lai (2020); Kumar & Bošnjak (2020), see also Margalit et al 2020;Lyutikov & Popov 2020;Lu et al 2020;Yu et al 2020;Katz 2020;Yang et al 2020;Yuan et al 2020, for models associated with soft gamma-ray repeaters), and old NSs under interaction with their companion (Wang et al (2016(Wang et al ( , 2018; Dai et al (2016); Zhang (2016, see also Dai 2020;Geng et al 2020, for models associated with soft gamma-ray repeaters) can be FRB progenitors.…”

Section: Introductionmentioning

confidence: 99%

The radio/X-ray burst from SGR 1935+2154: radiation mechanisms and the possible QPOs

Wang¹

2020

Preprint

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Recently, a fast radio burst (FRB)-like event is found to be associated with a Galactic magnetar, SGR 1935+2154, accompanied by an X-ray burst. We find this radio burst challenges the typical emission mechanisms involving magnetars, which includes coherent curvature radiation from charged bunches, fast magnetosonic (FMS) wave, synchrotron maser from shocks, and the pulsar-like mechanism for low-twist magnetars. More specifically, we find that (1) the X-rays are most-likely to be produced inside the magnetosphere. (2) For the coherent curvature radiation from the decay of Alfvén wave, it will generally predict a duration ( 0.1 ms) smaller than observations, because of the strong twists of magnetic field lines and the internal damping of Alfvén waves. (3) The FMS wave model predicts a very low emission frequency ν p ∼ 0.03 MHz ≪ GHz, unless it is produced inside the magnetosphere. But the absorption effect of the magnetospheric FMS wave model remains to be studied. ( 4) The synchrotron maser model is challenged, because observations show that the peaks in both X-ray and radio light curves are with the same temporal separation ∆t FRB = ∆t γ ≈ 0.03 s, while it would predict ∆t FRB ≪ ∆t γ . ( 5) It seems to be difficult to directly apply the low-twist pulsar-like mechanism to flaring magnetars, as magnetar activity can significantly deform the magnetosphere. ( 6) We discussed four possibilities to study radio burst properties for future observations, especially the possibility of high-frequency (0.5 − 2 ms) quasi-periodic oscillations in double/multiple-peaked FRBs.

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Section: Introductionmentioning

confidence: 99%

The radio/X-ray burst from SGR 1935+2154: radiation mechanisms and the possible QPOs

Wang¹

2020

Preprint

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“…• The trigger of QPOs in the neutron star crust is likely from internal, but an external trigger powered by infall of an asteroid is also possible (Dai 2020; Geng et al 2020), which might explain the rarity of the FRB-associated bursts. Such models, however, need to interpret the existence of QPOs already before the spikes associated with FRB pulses.…”

Section: Constraints On Theoretical Modelsmentioning

confidence: 99%

Quasi-periodic oscillations of the X-ray burst from the magnetar SGR J1935+2154 and associated with the fast radio burst FRB 200428

Li,

Ge,

Lin

et al. 2022

Preprint

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The origin(s) and mechanism(s) of fast radio bursts (FRBs), which are short radio pulses from cosmological distances, have remained a major puzzle since their discovery. We report a strong Quasi-Periodic Oscillation (QPO) of ∼40 Hz in the X-ray burst from the magnetar SGR J1935+2154 and associated with FRB 200428, significantly detected with the Hard X-ray Modulation Telescope (Insight-HXMT) and also hinted by the Konus-Wind data. QPOs from magnetar bursts have only been rarely detected; our 3.4 σ (p-value is 2.9e-4) detection of the QPO reported here reveals the strongest QPO signal observed from magnetars (except in some very rare giant flares), making this X-ray burst unique among magnetar bursts. The two X-ray spikes coinciding with the two FRB pulses are also among the peaks of the QPO. Our results suggest that at least some FRBs are related to strong oscillation processes of neutron stars. We also show that we may overestimate the significance of the QPO signal and underestimate the errors of QPO parameters if QPO exists only in a fraction of the time series of a X-ray burst which we use to calculate the Leahy-normalized periodogram.

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“…Similar behaviors between FRBs and solar type III radio bursts have been found (Zhang et al 2019). There are some theoretical works on this FRB (Margalit et al 2020a;Lu et al 2020;Lyutikov & Popov 2020;Dai 2020;Geng et al 2020;Katz 2020;Yu et al 2020;Yang et al 2020). In this paper, we focus on the synchrotron maser shock model proposed by Metzger et al (2019).…”

Section: Introductionmentioning

confidence: 99%

Understanding FRB 200428 in the synchrotron maser shock model: consistency and possible challenge

Zhang

Wang

et al. 2020

Preprint

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Recently, the discovery of Galactic FRB 200428 associated with a X-ray burst (XRB) of SGR 1935+2154 has built a bridge between FRBs and magnetar activities. In this paper, we assume that the XRB occurs in the magnetar magnetosphere. We show that the observational properties of FRB 200428 and the associated XRB are consistent with the predictions of synchrotron maser emission at ultrarelativistic magnetized shocks, including radiation efficiency, similar energy occurrence frequency distributions, and simultaneous arrive times. It requires that the upstream medium is a mildly relativistic baryonic shell ejected by a previous flare. The energy injection by flares responsible for the radio bursts will produce a magnetar wind nebula, which has been used to explain the persistent radio source associated FRB 121102. We find that the radio continuum around SGR 1935+2154 can be well understood in the magnetar wind nebula model, by assuming the same energy injection rate Ė ∝ t −1.37 as FRB 121102. The required baryonic mass is also estimated form the observations of FRB 121102 by GBT and FAST. By assuming the same radiation efficiency η ∼ 10 −5 , the total baryonic mass ejected from the central magnetar is about 0.005 solar mass. This value is much larger than the typical mass of a magnetar outer crust, but is comparable to the total mass of a magnetar crust.

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FRB 200428: an Impact between an Asteroid and a Magnetar

Cited by 3 publications

References 50 publications

The radio/X-ray burst from SGR 1935+2154: radiation mechanisms and the possible QPOs

The radio/X-ray burst from SGR 1935+2154: radiation mechanisms and the possible QPOs

Quasi-periodic oscillations of the X-ray burst from the magnetar SGR J1935+2154 and associated with the fast radio burst FRB 200428

Understanding FRB 200428 in the synchrotron maser shock model: consistency and possible challenge

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