Quasi-periodic sub-pulse structure as a unifying feature for radio-emitting neutron stars

Kramer, Michael; Liu, Kuo; Desvignes, Gregory; Karuppusamy, Ramesh; Stappers, Ben W.

doi:10.1038/s41550-023-02125-3

Cited by 6 publications

(2 citation statements)

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“…With periodicities between a dozen and more than 100 days found in repeating FRBs, there is now a consensus that the burst periodicity is associated with either the orbital periods of binary systems, with the companion being a degenerate star or massive star, or the precession of a magnetar (Levin et al 2020;Du et al 2021;Rajwade & van den Eijnden 2023). And the possible origin of an ultra-longperiod neutron star cannot be ruled out for FRBs with shorter periods (Beniamini et al 2020;Kramer et al 2023;Beniamini et al 2023).…”

Section: Possible Origin Of the Radio Emissionmentioning

confidence: 99%

A Candidate Period of 4.605 Days for FRB 20121102A and One Possible Implication of Its Origin

Li,

Gao,

et al. 2024

ApJ

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A firm establishment of the presence or the lack of periodicity in repeating fast radio bursts is crucial for determining their origins. Here, we compile 1145 radio bursts of FRB 20121102A with fluence larger than 0.15 Jy ms from observations using the Five-hundred-meter Aperture Spherical radio Telescope, the Arecibo Observatory, the Green Bank Telescope, the Effelsberg Telescope, the MeerKAT Telescope, the Lovell Telescope, the Deep Space Network 70 m radio telescopes, the Very Large Array, and the Westerbork Synthesis Radio Telescope, spanning the time interval of MJD 57175−58776. A quasi-period of 157.1 − 4.8 + 5.2 days and a candidate quasi-period of 4.605 − 0.010 + 0.003 days are found through the phase-folding probability binomial analysis. The former is consistent with previous findings and the latter is new. The 4.605 day periodicity is more obvious in high-energy bursts with fluence larger than 1 × 1038 erg. The presence of these (candidate) quasi-periods, together with the corresponding width of burst accumulation in the phase space, are consistent with the bursts originating from a binary degenerate star system with a close-by planet around the primary neutron star.

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Section: Possible Origin Of the Radio Emissionmentioning

confidence: 99%

A Candidate Period of 4.605 Days for FRB 20121102A and One Possible Implication of Its Origin

Li,

Gao,

et al. 2024

ApJ

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“…Some FRBs have been observed to exhibit quasi-periodicity, which does not appear to be related to a spin period (Chime/Frb Collaboration et al 2022;Pastor-Marazuela et al 2023). Observations of pulsars and magnetars have shown that quasi-periodic temporal structures can originate with frequencies orders of magnitude higher than the spin period (e.g., Kramer et al 2023), but such bursts present very differently in the polarization domain, showing flat PA curves in stark contrast to FRB 20210912A and FRB 20181112A. However, the existence of two remarkably similar FRBs suggests that at least a subclass of FRBs may originate in near-maximally rotating neutron stars, although identification of such events may not always be possible owing to various possible reasons discussed in Appendix F.…”

Section: A Possible Subclass Of Frbs?mentioning

confidence: 99%

The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?

Bera,

James,

Deller

et al. 2024

ApJL

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Fast radio bursts (FRBs) are brilliant short-duration flashes of radio emission originating at cosmological distances. The vast diversity in the properties of currently known FRBs and the fleeting nature of these events make it difficult to understand their progenitors and emission mechanism(s). Here we report high time resolution polarization properties of FRB 20210912A, a highly energetic event detected by the Australian Square Kilometre Array Pathfinder (ASKAP) in the Commensal Real-time ASKAP Fast Transients survey, which show intraburst position angle (PA) variation similar to Galactic pulsars and unusual variation of Faraday rotation measure (RM) across its two sub-bursts. The observed intraburst PA variation and apparent RM variation pattern in FRB 20210912A may be explained by a rapidly spinning neutron star origin, with rest-frame spin periods of ∼1.1 ms. This rotation timescale is comparable to the shortest known rotation period of a pulsar and close to the shortest possible rotation period of a neutron star. Curiously, FRB 20210912A exhibits a remarkable resemblance to the previously reported FRB 20181112A, including similar rest-frame emission timescales and polarization profiles. These observations suggest that these two FRBs may have similar origins.

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High-cadence monitoring of the emission properties of magnetar XTE J1810−197 with the Stockert radio telescope

Bause,

Herrmann,

Spitler

2024

A&A

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Context. Since the detection of a burst resembling a fast radio burst (FRB) from the Galactic magnetar SGR 1935+2154, magnetars have joined the set of favourable candidates for FRB progenitors. However, the emission mechanism of magnetars remains poorly understood. Aims. Observations of magnetars with a high cadence over extended timescales have allowed for their emission properties to be determined, in particular, their temporal variations. In this work, we present the results of the long-term monitoring campaign of the magnetar XTE J1810−197 since its second observed active phase from December 2018 until November 2021, with the Stockert 25 m radio telescope. Methods. We present a single pulse search method, improving on commonly used neural network classifiers thanks to the filtering of radio frequency interference based on its spectral variance and the magnetar’s rotation. Results. With this approach, we were able to lower the signal to noise ratio (S/N) detection threshold from 8 to 5. This allowed us to find over 115 000 spiky single pulses – compared to 56 000 from the neutral network approach. Here, we present the temporal variation of the overall profile and single pulses. Two distinct phases of different single pulse activity can be identified: phase 1 from December 2018 to mid-2019, with a few single pulses per hour, and phase 2 from September 2020 with hundreds of single pulses per hour (with a comparable average flux density). We find that the single pulse properties and folded profile in phase 2 exhibit a change around mid-March 2021. Before this date, the folded profile consists of a single peak and single pulses, with fluences of up to 1000 Jyms and a single-peaked width distribution at around 10 ms. After mid-March 2021, the profile consists of a two peaks and the single pulse population shows a bimodal width distribution with a second peak at 1 ms and fluences of up to 500 Jyms. We also present asymmetries in the phase-resolved single pulse width distributions beginning to appear in 2020, where the pulses arriving earlier in the rotational phase appear wider than those appearing later. This asymmetry persists despite the temporal evolution of the other single pulse and emission properties. Conclusions. We argue that a drift in the emission region in the magnetosphere may explain this observed behaviour. Additionally, we find that the fluence of the detected single pulses depends on the rotational phase and the highest fluence is found in the centre of the peaks in the profile. While the majority of the emission can be linked to the detected single pulses, we cannot exclude another weak mode of emission. In contrast to the pulses from SGR 1935+2154, we have not found any spectral feature or bursts with energies in the order of magnitude of an FRB during our observational campaign. Therefore, the question of whether this magnetar is capable of emitting such highly energetic bursts remains open.

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Quasi-periodic sub-pulse structure as a unifying feature for radio-emitting neutron stars

Cited by 6 publications

References 84 publications

A Candidate Period of 4.605 Days for FRB 20121102A and One Possible Implication of Its Origin

A Candidate Period of 4.605 Days for FRB 20121102A and One Possible Implication of Its Origin

The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?

High-cadence monitoring of the emission properties of magnetar XTE J1810−197 with the Stockert radio telescope

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