Radio Emission from Pulsar Wind Nebulae without Surrounding Supernova Ejecta: Application to FRB 121102

Dai, Z. G.; Wang, Jie-Shuang; Yu, Yun-Wei

doi:10.3847/2041-8213/aa6745

Cited by 60 publications

(61 citation statements)

References 55 publications

(72 reference statements)

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“…There are many suggestions for the FRB mechanism, including soft gamma-ray repeats (e.g., Popov & Postnov 2010;Kulkarni et al 2014;Lyubarsky 2014; see however Tendulkar et al 2016), Galactic stars (e.g., Maoz et al 2015), pulsars (e.g., Lyutikov et al 2016;Katz 2017a), magnetars (e.g., Metzger et al 2017), pulsar wind nebulae (e.g., Dai, Wang & Yu 2017), active galactic nuclei (Katz 2017b), and more. Based on the FRB 121102 persistent source luminosity, spectrum, angular size, and the FRBs constant dispersion measure (DM) over a year time scale, Waxman (2017) inferred the properties of the emitting region.…”

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confidence: 99%

A Search for FRB 121102-like Persistent Radio-luminous Sources—Candidates and Implications for the FRB Rate and Searches

Ofek

2017

ApJ

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The localization of the repeating fast radio burst (FRB), FRB 121102, suggests that it is associated with a persistent radio-luminous compact source in the FRB host galaxy. Using the FIRST radio catalog, I present a search for luminous persistent sources in nearby galaxies, with radio luminosities > 10% of the FRB 121102 persistent source luminosity. The galaxy sample contains about 30% of the total galaxy g-band luminosity within < 108 Mpc, in a footprint of 10,600 deg 2 . After rejecting sources likely due to active galactic nuclei activity or background sources, I remain with 11 candidates that are presumably associated with galactic disks or star formation regions. At least some of these candidates are likely to be due to chance alignment. In addition, I find 85 sources within 1 ′′ of galactic nuclei. Assuming the radio persistent sources are not related to galactic nuclei and that they follow the galaxy g-band light, the 11 sources imply a 95% confidence upper limit on the space density of luminous persistent sources of < ∼ 5 × 10 −5 Mpc −3 , and that at any given time only a small fraction of galaxies host a radio luminous persistent source ( < ∼ 10 −3 L −1 * ). Assuming persistent sources life time of 100 yr, this implies a birth rate of < ∼ 5 × 10 −7 yr −1 Mpc −3 . Given the FRB volumetric rate, and assuming that all FRBs repeat and are associated with persistent radio sources, this sets a lower limit on the rate of FRB events per persistent source of > ∼ 0.8 yr −1 . I argue that these 11 candidates are good targets for FRB searches and I estimate the FRB event rate from these candidates.

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confidence: 99%

A Search for FRB 121102-like Persistent Radio-luminous Sources—Candidates and Implications for the FRB Rate and Searches

Ofek

2017

ApJ

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“…1. Since the constraints are drawn from the properties of the burst only, the results do not depend on the properties of the persistent source and the circumburst environment discussed in other papers (Metzger et al 2017;Lyutikov 2017;Kashiyama & Murase 2017;Cao et al 2017;Dai et al 2017). The determined parameters within narrow region are the dipole magnetic field B d ∼ 10 13 G, and the initial period P i < ∼ 3 ms, if the emission is isotropically emitted (f Ω ∼ 1) and temporal evolution follows the dipole radiation formula (n = 3).…”

Section: Discussionmentioning

confidence: 99%

“…The propagation effects on the radio emission and the possible association of persistent radio source could give significant constraints on the model for FRB 121102 (Metzger et al 2017;Lyutikov 2017;Kashiyama & Murase 2017;Cao et al 2017;Dai et al 2017). For example, if the injected energy from an NS changes the dynamics of surrounded materials, the observed DM could give constraints on the NS parameters.…”

Section: Constraints On Grp-like Emission Modelmentioning

confidence: 99%

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Constraints on pulsed emission model for repeating FRB 121102

Kisaka

Enoto

Shibata

2017

Publications of the Astronomical Society of Japan

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Recent localization of the repeating Fast Radio Burst (FRB) 121102 revealed the distance of its host galaxy and luminosities of the bursts. We investigated constraints on the young neutron star (NS) model, that (a) the FRB intrinsic luminosity is supported by the spin-down energy, and (b) the FRB duration is shorter than the NS rotation period. In the case of a circular cone emission geometry, conditions (a) and (b) determine the NS parameters within very small ranges, compared with that from only condition (a) discussed in previous works. Anisotropy of the pulsed emission does not affect the area of the allowed parameter region by virtue of condition (b). The determined parameters are consistent with those independently limited by the properties of the possible persistent radio counterpart and the circumburst environments such as surrounding materials. Since the NS in the allowed parameter region is older than the spin-down timescale, the hypothetical GRP-like model expects a rapid radio flux decay of < ∼ 1 Jy within a few years as the spin-down luminosity decreases. The continuous monitoring will give a hint of discrimination of the models. If no flux evolution will be seen, we need to consider an alternative model, e.g., the magnetically powered flare.

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“…The parameters of the theoretical curves used for each event are listed in Table 1. its host galaxy and persistent radio counterpart. Several authors claim that a high spin-down luminosity and/or small ejecta mass are favored to explain the observed characteristics of FRB 121102 (Kashiyama & Murase 2017;Metzger et al 2017;Kisaka et al 2017;Katz 2017;Dai et al 2017;Piro & Burke-Spolaor 2017;Waxman 2017).…”

Section: Connection Between Fast Radio Bursts and Double Pulsar Systems?mentioning

confidence: 99%

Rapidly Rising Optical Transients from the Birth of Binary Neutron Stars

Hotokezaka

Kashiyama

Murase

2017

ApJ

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We study optical counterparts of a new-born pulsar in a double neutron star system like PSR J0737-3039A/B. This system is believed to have ejected a small amount of mass of O(0.1M ⊙ ) at the second core-collapse supernova. We argue that the initial spin of the new-born pulsar can be determined by the orbital period at the time when the second supernova occurs. The spin angular momentum of the progenitor is expected to be similar to that of the He-burning core, which is tidally synchronized with the orbital motion, and then the second remnant may be born as a millisecond pulsar. If the dipole magnetic field strength of the nascent pulsar is comparable to that inferred from the current spin-down rate of PSR J0737-3039B, the initial spin-down luminosity is comparable to the luminosity of super-luminous supernovae. We consider thermal emission arising from the supernova ejecta driven by the relativistic wind from such a new-born pulsar. The resulting optical light curves have a rise time of ∼ 10 days and peak luminosity of ∼ 10 44 erg/s. The optical emission may last for a month to several months, due to the reprocessing of X-rays and UV photons via photoelectric absorption. These features are broadly consistent with those of the rapidly rising optical transients. The high spin-down luminosity and small ejecta mass are favorable for the progenitor of the repeating fast radio burst, FRB 121102. We discuss a possible connection between newborn double pulsars and fast radio bursts.

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Radio Emission from Pulsar Wind Nebulae without Surrounding Supernova Ejecta: Application to FRB 121102

Cited by 60 publications

References 55 publications

A Search for FRB 121102-like Persistent Radio-luminous Sources—Candidates and Implications for the FRB Rate and Searches

A Search for FRB 121102-like Persistent Radio-luminous Sources—Candidates and Implications for the FRB Rate and Searches

Constraints on pulsed emission model for repeating FRB 121102

Rapidly Rising Optical Transients from the Birth of Binary Neutron Stars

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