Very-high-frequency oscillations in the main peak of a magnetar giant flare

Castro‐Tirado, Alberto J.; Østgaard, Nikolai; Göǧüş, E.; Sánchez-Gil, M. Carmen; Pascual-Granado, J.; Reglero, Víctor; Mezentsev, A. N.; Gabler, Michael; Marisaldi, M.; Neubert, Torsten; Budtz-Jørgensen, Carl; Lindanger, Anders; Sarria, David; Kuvvetli, I.; Cerdá–Durán, P.; Navarro‐González, J.; Font, José A.; Zhang, B.-B.; Lund, N.; Oxborrow, C. A.; Brandt, S.; Caballero‐García, M. D.; Carrasco-García, Irene María; Castellón, A.; Tirado, M. A. Castro; Christiansen, F.; Eyles, C. J.; Fernández-García, E.; Genov, Georgi; Guziy, S.; Hu, Y. D.; Guelbenzu, A. Nicuesa; Peng, Zong-Kai; Pulgar, C. Pérez del; Terol, A. J. Reina; Rodrı́guez, E.; Sánchez-Ramírez, R.; Sun, Tianrui; Ullaland, K.

doi:10.1038/s41586-021-04101-1

Cited by 42 publications

(46 citation statements)

References 47 publications

(76 reference statements)

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“…A series of short-lived QPOs with center frequencies of ∼10-600 Hz were found during the giant flares of SGR 1806−20 and SGR 1900 +14 (Israel et al 2005;Strohmayer & Watts 2005, 2006Huppenkothen et al 2014c;Miller et al 2019). Recently, Castro-Tirado et al (2021) reported two broad high-frequency QPOs in the main peak of an extragalactic giant flare lasting for 3.5 ms. During the short bursts from SGR J1550−5418, which are in the same category as those from SGR J1935+2154, a weak QPO signal at ∼260 Hz was possibly found in a single burst (Huppenkothen et al 2014b). Using the same data but stacking some short bursts together, more significant QPOs centered at ∼93 and ∼127 Hz, which are close to those found in giant flares, were reported (Huppenkothen et al 2014b).…”

Section: Introductionmentioning

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

Lin

et al. 2022

ApJ

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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 at by the Konus–Wind data. QPOs from magnetar bursts have only been rarely detected; our 3.4σ (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 an X-ray burst that we use to calculate the Leahy-normalized periodogram.

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Section: Introductionmentioning

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

Lin

et al. 2022

ApJ

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“…First, the derived isotropic kinetic energy is ∼ 10 49 -10 50 erg, which is more than three orders of magnitude larger than the kinetic energy inferred by the typical GFs. For example, GRB 200415A is one of the most energetic extragalactic GFs, with the isotropic energy released in the initial pulse and following tail being ∼10 46 erg Zhang et al 2020b;Castro-Tirado et al 2021;Fermi-LAT Collaboration et al 2021;Roberts et al 2021;Svinkin et al 2021). GRB 200415A is also the first GF accompanied by GeV emission that is generally believed to originate from the GF afterglow Zhang et al 2020b;Fermi-LAT Collaboration et al 2021).…”

Section: Can the Giant Flare Afterglow Model Explainmentioning

confidence: 99%

AT2020hur: A Possible Optical Counterpart of FRB 180916B

Zhong

et al. 2022

ApJ

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The physical origin of fast radio bursts (FRBs) remains unclear. Finding multiwavelength counterparts of FRBs can provide a breakthrough for understanding their nature. In this work, we perform a systematic search for astronomical transients whose positions are consistent with FRBs. We find an unclassified optical transient AT2020hur (α = 01h58m00.ˢ750 ± 1″, δ = 65 ° 43 ′ 00 .″ 30 ± 1 ″ ) that is spatially coincident with the repeating FRB 180916B (α = 01h58m00.ˢ7502 ± 2.3 mas, δ = 65 ° 43 ′ 00 .″ 3152 ± 2.3 mas; Marcote et al. 2020). The chance possibility of the AT2020hur–FRB 180916B association is about 0.04%, which corresponds to a significance of 3.5σ. We develop a giant flare (GF) afterglow model to fit AT2020hur. Although the GF afterglow model can interpret the observations of AT2020hur, the derived kinetic energy of such a GF is at least three orders of magnitude larger than that of a typical GF, and a lot of fine-tuning and coincidences are required for this model. Another possible explanation is that AT2020hur might consist of two or more optical flares originating from the FRB source, e.g., fast optical bursts produced by the inverse Compton scattering of FRB emission. Besides, AT2020hur is located in one of the activity windows of FRB 180916B, which provides independent support for the association. This coincidence may be due to the optical counterparts being subject to the same periodic modulation as FRB 180916B, as implied by the prompt FRB counterparts. Future simultaneous observations of FRBs and their optical counterparts may help to reveal their physical origin.

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“…First, the derived isotropic kinetic energy is ∼ 10 49 − 10 50 erg, which is more than 3 orders of magnitude larger than the kinetic energy inferred by the typical GFs. For example, GRB 200415A is one of the most energetic extragalactic GFs with an isotropic energy released in the initial pulse and following tail of ∼ 10 46 erg Zhang et al 2020b;Castro-Tirado et al 2021;Fermi-LAT Collaboration et al 2021;Roberts et al 2021;Svinkin et al 2021).…”

Section: Can Giant Flare Afterglow Model Explainmentioning

confidence: 99%

AT2020hur: A Possible Optical Counterpart of FRB 180916B

Li,

Zhong

et al. 2022

Preprint

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The physical origin of fast radio bursts (FRBs) remains unclear. Finding multiwavelength counterparts of FRBs can be a breakthrough in understanding their nature. In this work, we perform a systematic search for astronomical transients (ATs) whose positions are consistent with FRBs. We find an unclassified optical transient AT2020hur (α = 01 h 58 m 00.750 s ± 1 arcsec, δ = 65 • 43 ′ 00.30 ′′ ± 1 arcsec; Lipunov et al. 2020) that is spatially coincident with the repeating FRB 180916B (α = 01 h 58 m 00.7502 s ± 2.3 mas, δ = 65 • 43 ′ 00.3152 ′′ ± 2.3 mas; Marcote et al. 2020). The chance possibility for the AT2020hur-FRB 180916B association is about 0.04%, which corresponds to a significance of 3.5σ. We develop a giant flare afterglow model to fit AT2020hur. Although the giant flare afterglow model can interpret the observations of AT2020hur, the derived kinetic energy of such a GF is at least three orders of magnitude larger than that of the typical GF, and there is a lot of fine tuning and coincidences required for this model. Another possible explanation is that AT2020hur might consist of two or more optical flares originating from the FRB source, e.g. fast optical bursts produced by the inverse Compton scattering of FRB emission. Besides, AT2020hur is located in one of the activity windows of FRB 180916B, which is an independent support for the association. This coincidence may be due to the reason that the optical counterpart is subject to the same periodic modulation as FRB 180916B, as implied by the prompt FRB counterparts. Future simultaneous observations of FRBs and their optical counterparts may help reveal their physical origin.

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Very-high-frequency oscillations in the main peak of a magnetar giant flare

Cited by 42 publications

References 47 publications

Quasi-periodic Oscillations of the X-Ray Burst from the Magnetar SGR J1935–2154 and Associated with the Fast Radio Burst FRB 200428

Quasi-periodic Oscillations of the X-Ray Burst from the Magnetar SGR J1935–2154 and Associated with the Fast Radio Burst FRB 200428

AT2020hur: A Possible Optical Counterpart of FRB 180916B

AT2020hur: A Possible Optical Counterpart of FRB 180916B

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