Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

Dai, Z. G.; Zhong, S. Q.

doi:10.48550/arxiv.2003.04644

Cited by 3 publications

(3 citation statements)

References 38 publications

(56 reference statements)

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“…The ∼ 16-day periodicity of FRB 180916.J0158+65 Marcote et al (2020b) may require a binary systems (e.g. Ioka & Zhang 2020;Lyutikov et al 2020;Katz 2020;Dai & Zhong 2020). These systems may have a host galaxy or local environment similar to intermediate stellar populations.…”

Section: Resultsmentioning

confidence: 99%

A comparative study of host galaxy properties between Fast Radio Bursts and stellar transients

Li,

Zhang

2020

Preprint

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Recent localizations of Fast Radio Bursts and identifications of their host galaxies confirmed their extragalactic origin. While FRB 121102 resides in the bright region of a dwarf star forming galaxy, other FRBs reside in more massive galaxies and are related to older stellar populations. We compare the host galaxy properties of the five FRBs with those of several types of stellar transients: from young to old population, long duration gamma ray bursts (LGRBs), superluminous supernovae (SLSNe), Type Ib/Ic supernovae (SN Ibc), Type II supernovae (SN II), type Ia supernovae (SN Ia), and short duration gamma ray bursts (SGRBs). We find that as a whole sample, the stellar mass and star formation rate of the five FRB host galaxies prefer a medium to old population, and are against a young population similar to LGRBs and SLSNe by a null probability 0.05. Individually, the FRB 121102 host is consistent with that of young population objects, especially SLSNe; the FRB 180924 environment is similar to that of SGRBs; and the FRB 190523 environment is similar to those of SN Ia or SGRBs. These results are consistent with the magnetar engine model for FRBs, if both magnetars produced from extreme explosions (GRBs/SLSNe) and from regular channels (e.g. those producing Galactic magnetars) can produce FRBs.

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Section: Resultsmentioning

confidence: 99%

A comparative study of host galaxy properties between Fast Radio Bursts and stellar transients

Li,

Zhang

2020

Preprint

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“…The reported periodicity is far too long to be ascribed to a neutron star's rotational frequency, and triggered a wealth of alternative hypotheses, such as orbital effects (Lyutikov et al 2020;Ioka & Zhang 2020) or various kinds of precessional effects (Yang & Zou 2020;Levin et al 2020;Zanazzi & Lai 2020;Gu et al 2020) or other secular semi-periodic cyclic phenomena, e.g. the source traveling across an asteroid belt (Dai & Zhong 2020). Most of these models revisited concepts developed for the modeling of the original RFRB (for a review see Platts et al 2019), tuned to a ∼ 16 days periodicity.…”

Section: Introductionmentioning

confidence: 99%

The lowest frequency Fast Radio Bursts: Sardinia Radio Telescope detection of the periodic FRB 180916 at 328 MHz

Pilia,

Burgay,

Possenti

et al. 2020

Preprint

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We report on the lowest-frequency detection to date of three bursts from FRB 180916.J0158+65, observed at 328 MHz with the Sardinia Radio Telescope (SRT). The SRT observed the periodic repeater FRB 180916.J0158+65 for five days from Feb. 20, 2020 to Feb. 24, 2020 during a time interval of active radio bursting, and detected the three bursts during the first hour of observation; no more bursts were detected during the remaining ∼ 30 hours. Simultaneous SRT observations at 1548 MHz did not detect any bursts. Bursts fluences are in the range 37 to 13 Jy ms. No relevant scattering is observed for these bursts.We also present the results of the multi-wavelength campaign that we performed on FRB 180916.J0158+65, during the ∼ 5 days of the active window. Observations on different time spans were performed simultaneously with the SRT observations with the Northern Cross at 408 MHz, with XMM-Newton, NICER, INTEGRAL, AGILE and with the TNG and two optical telescopes in Asiago, which are equipped with fast photometers. XMM-Newton obtained data simultaneously with the three bursts detected by the SRT and determined a luminosity upper limit in the 0.3-10 keV energy range of ∼ 10 45 erg s −1 for the burst emission. AGILE obtained data simultaneously with the first burst and determined a fluence upper limit in the MeV range for millisecond timescales of 10 −8 erg cm −2 .Our results sensibly constrain the broad-band emission from FRB 180916.J0158+65, and provide the best limits so far for the electromagnetic response to the radio bursting of this remarkable source of fast radio bursts.

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“…NS and massive star binary to interpret the periodicity of FRB 180916, but they proposed that the observed periodicity is due to the orbital phase-dependent modulation of the absorption conditions in the massive star's wind, instead of intrinsic to the FRBs' source. Dai & Zhong (2020) propose that periodically repeating FRB might be produced from an old-aged pulsar traveling through the asteroid belts of its companion star, so that the periodically repeating FRBs would provide a unique probe of extragalactic asteroid belts. Gu et al (2020) suggested that FRB 180916 is produced by a NS-white dwarf (WD) binary system when the WD fills its Roche lobe at the pericenter, so that the mass transfer from the WD to the NS resulting in multiple radio bursts.…”

Section: Introductionmentioning

confidence: 99%

What binary systems are the most likely sources for periodically repeating FRBs?

Zhang,

Gao

2020

Preprint

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The newly discovered 16.35 days period for repeating FRB 180916.J0158+65 provides an essential clue for understanding the sources and emission mechanism of repeating FRBs. Many models propose that the periodically repeating FRBs might be related to binary star systems that contain at least one neutron star (NSC-FRB system). It has been suggested that the NS "combed" by the strong wind from a companion star might provide a solution. Following the "Binary Comb" model, we use the population synthesis method to study in detail the properties of the companion stars and the nature of NSC-FRB systems. Our main findings are: 1) the companion star is most likely to be a B-type star; 2) the period of 16 days of FRB 180916 happens to fall in the most probable period range, which may explain why FRB 180916 was the first detected periodically repeating FRB, and we expect to observe more periodically repeating FRBs with periods around 10-30 days; 3) the birth rate for NSC-FRB system is large enough to fulfill the event rate requirement set by the observation of FRB 180916, which supports the proposal that NSC-FRB can provide one significant channel for producing periodically repeating FRBs.

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Periodic Fast Radio Bursts as a Probe of Extragalactic Asteroid Belts

Cited by 3 publications

References 38 publications

A comparative study of host galaxy properties between Fast Radio Bursts and stellar transients

A comparative study of host galaxy properties between Fast Radio Bursts and stellar transients

The lowest frequency Fast Radio Bursts: Sardinia Radio Telescope detection of the periodic FRB 180916 at 328 MHz

What binary systems are the most likely sources for periodically repeating FRBs?

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