Periodic activity from fast radio burst FRB180916 explained in the frame of the orbiting asteroid model

Voisin, Guillaume; Mottez, Fabrice; Zarka, Philippe

doi:10.1093/mnras/stab2622

Cited by 9 publications

(7 citation statements)

References 70 publications

(100 reference statements)

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“…The average DM is 349 cm −3 pc, and the average RM is −108 rad m −2 . The activities of this FRB source show a period of 16.35 days (CHIME/FRB Collaboration et al 2020b;Voisin et al 2021). It is located in a nearby massive spiral galaxy at a redshift of z = 0.0337.…”

Section: Methodsmentioning

confidence: 95%

A Comprehensive Analysis of Repeating Fast Radio Bursts

Hu 胡,

Huang 黄

2023

ApJS

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Nearly 700 fast radio burst (FRB) sources have been detected so far, of which 29 are found to burst out repeatedly. Although a firm connection between at least some FRBs and magnetars has been established, the trigger mechanism and radiation process in these enigmatic phenomena are still highly controversial. In this study, we build a sample of 16 repeating FRBs from which at least five bursts have been detected, including the most active four repeaters of FRBs 20121102A, 20180916B, 20190520B, and 20201124A. Various key parameters of their bursts are collected from the literature, which include the arrival time, pulse width, dispersion measure (DM), Faraday rotation measure (RM), bandwidth, waiting time, peak flux, and fluence. The distribution and time evolution of these parameters are investigated. Potential correlations between various parameter pairs are also extensively explored. The behaviors of different repeaters are then compared. It is found that the DM of FRB 20121102A seems to increase continuously on a long timescale. While the DM of most repeaters varies in a narrow range of ±3 cm−3 pc, FRB 20190520B is found to have a large variation range of ±12 cm−3 pc. The RM evolves with time in a much more chaotic behavior in different repeaters. A linear correlation is found between the absolute mean RM and DMHost, which may provide a method to estimate the redshift of FRBs. Generally, the waiting time shows a similar bimodal distribution for the active repeating sources. The implications of these features to the underlying physics are discussed.

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Section: Methodsmentioning

confidence: 95%

A Comprehensive Analysis of Repeating Fast Radio Bursts

Hu 胡,

Huang 黄

2023

ApJS

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“…FRB 20180916B -16 days (Chime/Frb Collaboration et al 2020) and FRB 20121102A -160 days (Rajwade et al 2020;Cruces et al 2021;. The theoretical interpretations for these long cycles for FRBs include binary systems (Ioka & Zhang 2020;Zhang & Gao 2020;Sridhar et al 2021), magnetar precession (Yang & Zou 2020;Levin et al 2020;Zanazzi & Lai 2020;Sob'yanin 2020;Tong et al 2020), asteroid interactions Dai & Zhong (2020); Voisin et al (2021); Du et al (2021), and slow rotating magnetars (Beniamini et al 2020).…”

Section: Introductionmentioning

confidence: 99%

FAST Observations of an Extremely Active Episode of FRB 20201124A. IV. Spin Period Search

Niu

Zhu

Zhang

et al. 2022

Res. Astron. Astrophys.

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We report the properties of more than 800 bursts detected from the repeating fast radio burst (FRB) source FRB 20201124A with the Five-hundred-meter Aperture Spherical radio telescope (FAST) during an extremely active episode on UTC September 25th-28th, 2021 in a series of four papers. In this fourth paper of the series, we present a systematic search of the spin period and linear acceleration of the source object from both 996 individual pulse peaks and the dedispersed time series. No credible spin period was found from this data set. We rule out the presence of significant periodicity in the range between 1 ms to 100 s with a pulse duty cycle < 0.49±0.08 (when the profile is defined by a von-Mises function, not a boxcar function) and linear acceleration up to 300 m s^{−2} in each of the four one-hour observing sessions, and up to 0.6 m s^{−2} in all 4 days. These searches contest theoretical scenarios involving a 1 ms to 100 s isolated magnetar/pulsar with surface magnetic field < 10^15 G and a small duty cycle (such as in a polar-cap emission mode) or a pulsar with a companion star or black hole up to 100 M⊙ and Pb > 10 hours. We also perform a periodicity search of the fine structures and identify 53 unrelated millisecond-timescale ”periods” in multi-components with the highest significance of 3.9 σ. The ”periods” recovered from the fine structures are neither consistent nor harmonically related. Thus they are not likely to come from a spin period. We caution against claiming spin periodicity with significance below ∼ 4 σ with multi-components from one-off FRBs. We discuss the implications of our results and the possible connections between FRB multi-components and pulsar micro-structures.

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“…Several kinds of models have been proposed to explain the periodic activities (for a review, see Xiao et al 2021). First, FRBs occur in a binary system containing a stellar compact object (a neutron star (NS) or a black hole (BH)), where the observed period corresponds to the orbital period (Dai et al 2016;Zhang 2017;Dai & Zhong 2020;Gu et al 2020;Deng et al 2021;Geng et al 2021;Kuerban et al 2021;Voisin et al 2021;Wada et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Effects of Gravitational-wave Radiation of Eccentric Neutron Star–White Dwarf Binaries on the Periodic Activity of Fast Radio Burst Sources

Chen

et al. 2022

ApJ

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We revisit the eccentric neutron star (NS)–white dwarf (WD) binary model for the periodic activity of fast radio burst (FRB) sources, by including the effects of gravitational-wave (GW) radiation. In this model, the WD fills its Roche lobe at the periastron and mass transfer occurs from the WD to the NS. The accreted materials can be fragmented and arrive at the NS episodically, resulting in multiple bursts through curvature radiation. Consequently, the WD may be kicked away owing to the conservation of angular momentum. To initiate the next mass transfer, the WD has to refill its Roche lobe through GW radiation. In this scenario, whether the periodic activity can show up relies on three timescales, i.e., the orbital period P orb, the timescale T GW for the Roche lobe to be refilled, and the time span T frag for all the episodic events corresponding to each mass-transfer process. Only when the two conditions T GW ≲ P orb and T frag < P orb are both satisfied, the periodic activity will manifest itself and the period should be equal to P orb. In this spirit, the periodic activity is more likely to show up for relatively long periods (P orb ≳ several days). Thus, it is reasonable that FRBs 180916 and 121102, the only two sources having been claimed to manifest periodic activity, both correspond to relatively long periods.

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Periodic activity from fast radio burst FRB180916 explained in the frame of the orbiting asteroid model

Cited by 9 publications

References 70 publications

A Comprehensive Analysis of Repeating Fast Radio Bursts

A Comprehensive Analysis of Repeating Fast Radio Bursts

FAST Observations of an Extremely Active Episode of FRB 20201124A. IV. Spin Period Search

Effects of Gravitational-wave Radiation of Eccentric Neutron Star–White Dwarf Binaries on the Periodic Activity of Fast Radio Burst Sources

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