Pulsar-Wind Nebulae and Magnetar Outflows: Observations at Radio, X-Ray, and Gamma-Ray Wavelengths

Reynolds, Stephen P.; Pavlov, G. G.; Kargaltsev, Oleg; Klingler, N. J.; Renaud, M.; Mereghetti, S.

doi:10.1007/978-94-024-1292-5_7

Cited by 4 publications

(6 citation statements)

References 175 publications

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“…Alternatively, the association of FRB 121102 with a persistent radio source has been used to argue that the radio bursts are produced by a young magnetar powering a luminous wind nebula 13,48 . This model is not well motivated by Galactic examples, since the most luminous (non-magnetar powered) Galactic pulsar wind nebula is only 2 × 10 −6 times as luminous as the persistent source coincident with FRB 121102, and Galactic magnetars have no detectable persistent radio wind nebulae 49,50 . Also, while giant flares from magnetars can produce relativistic outflows 51 , an upper limit on the RM from one such outburst 52 is 4 orders of magnitude below that observed for FRB 121102.…”

Section: Constraints On the Properties Of The Faraday Regionmentioning

confidence: 99%

An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102

Michilli

Seymour

Hessels

et al. 2018

Nature

518

668

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Fast radio bursts (FRBs) are millisecond-duration, extragalactic radio flashes of unknown physical origin [1][2][3] . FRB 121102, the only known repeating FRB source [4][5][6] , has been localized to a star-forming region in a dwarf galaxy 7-9 at redshift z = 0.193, and is spatially coincident with a compact, persistent radio source 7,10 . The origin of the bursts, the nature of the persistent source, and the properties of the local environment are still debated. Here we present bursts that show ∼100% linearly polarized emission at a very high and variable Faraday rotation measure in the source frame: RM src = +1.46 × 10 5 rad m −2 and +1.33 × 10 5 rad m −2 at epochs separated by 7 months, in addition to narrow ( 30 µs) temporal structure. The large and variable rotation measure demonstrates that FRB 121102 is in an extreme and dynamic magneto-ionic environment, while the short burst durations argue for a neutron star origin. Such large rotation measures have, until now, only been observed 11,12 in the vicinities of massive black holes (M BH 10 4 M ). Indeed, the properties of the persistent radio source are compatible with those of a low-luminosity, accreting massive black hole 10 . The bursts may thus come from a neutron star in such an environment. However, the observed properties may also be explainable in other models, such as a highly magnetized wind nebula 13 or supernova remnant 14 surrounding a young neutron star. 2Using the 305-m William E. Gordon Telescope at the Arecibo Observatory, we detected 16 bursts from FRB 121102 at radio frequencies from 4.1 − 4.9 GHz (Table 1). The data recorder provided complete polarization parameters with 10.24-µs time resolution. See Methods and Extended Data Figs. 1-6 for observation and analysis details.The 4.5-GHz bursts have typical widths 1 ms, which are narrower than the 2 to 9-ms bursts previously detected at lower frequencies 5,15 . In some cases they show multiple components and structure close to the sampling time of the data. Burst #6 is particularly striking, with a width of 30 µs, which constrains the size of the emitting region to 10 km, modulo geometric and relativistic effects. Evolution in burst morphology with frequency complicates the determination 5 of dispersion measure (DM = d 0 n e (l) dl), but aligning the narrow component in Burst #6 results in DM= 559.7 ± 0.1 pc cm −3 , which is consistent 4,5,15,16 with other bursts detected since 2012, and suggests that any bona fide dispersion measure variations are at the 1% level.After correcting for Faraday rotation, and accounting for ∼2% depolarization from the finite channel widths, the bursts are consistently ∼100% linearly polarized (Fig. 1). The polarization angles PA = PA ∞ + θ (where PA ∞ is a reference angle at infinite frequency, θ = RMλ 2 is the rotation angle of the electric field vector and λ is the observing wavelength) are flat across the observed frequency range and burst envelopes (∆PA 5 • ms −1 ). This could mean that the burst durations reflect the timescale of the emission process and n...

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Section: Constraints On the Properties Of The Faraday Regionmentioning

confidence: 99%

An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102

Michilli

Seymour

Hessels

et al. 2018

Nature

518

668

View full text Add to dashboard Cite

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“…Flaring from the reverse shock could lead to additional (lower-energy) γ-ray emission, and the interaction between the GRB and the ejecta could lead to broadband afterglow emission lasting days to weeks (Kulkarni et al, 2015;Murase et al, 2016;Lyutikov and Lorimer, 2016). The quasisteady nebular emission of the magnetar wind nebula itself may be difficult to detect (Murase et al, 2016;Reynolds et al, 2017). X-rays are able to penetrate the ejecta, but only on a 100 year timescale, and are therefore unlikely to be detected (Margalit et al, 2018).…”

Section: Magnetar Wind Bubble (Clustered Flaresmentioning

confidence: 99%

A living theory catalogue for fast radio bursts

et al. 2019

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At present, we have almost as many theories to explain Fast Radio Bursts as we have Fast Radio Bursts observed. This landscape will be changing rapidly with CHIME/FRB, recently commissioned in Canada, and HIRAX, under construction in South Africa. This is an opportune time to review existing theories and their observational consequences, allowing us to efficiently curtail viable astrophysical models as more data becomes available. In this article we provide a currently up to date catalogue of the numerous and varied theories proposed for Fast Radio Bursts so far. We also launched an online evolving repository for the use and benefit of the community to dynamically update our theoretical knowledge and discuss constraints and uses of Fast Radio Bursts.

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“…The panels are numbered in accordance with tables 1 and 2. Chandra images of some of these objects are also shown in Reynolds et al (2017). morphologies (cf.…”

Section: Magnetic Fields and Related Parametersmentioning

confidence: 99%

“…The white arrows show the directions of pulsar proper motion, and the green arrow shows the bending in the Lighthouse Nebula outflow (inset). Chandra images of some of these objects are also shown in Reynolds et al (2017). can be estimated as γ ∼ 2 × 10 8 (E/1 keV) 1/2 (B ISM /5 µG) −1/2 , where B ISM is the ambient magnetic field, and E is the synchrotron photon energy that reaches at least 8 keV for the Lighthouse, Guitar and J1509-5058 PWNe.…”

Section: Misaligned Outflowsmentioning

confidence: 99%

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Pulsar wind nebulae created by fast-moving pulsars

et al. 2017

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We review multiwavelength properties of pulsar wind nebulae created by supersonically moving pulsars and the effects of pulsar motion on the pulsar wind nebulae morphologies and the ambient medium. Supersonic pulsar wind nebulae are characterized by bow-shaped shocks around the pulsar and/or cometary tails filled with the shocked pulsar wind. In the past several years significant advances in supersonic pulsar wind nebula studies have been made in deep observations with the Chandra and XMM-Newton X-ray observatories and the Hubble Space Telescope. In particular, these observations have revealed very diverse supersonic pulsar wind nebula morphologies in the pulsar vicinity, different spectral behaviours of long pulsar tails, the presence of puzzling outflows misaligned with the pulsar velocity and far-UV bow shocks. Here we review the current observational status focusing on recent developments and their implications.

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Pulsar-Wind Nebulae and Magnetar Outflows: Observations at Radio, X-Ray, and Gamma-Ray Wavelengths

Cited by 4 publications

References 175 publications

An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102

An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102

A living theory catalogue for fast radio bursts

Pulsar wind nebulae created by fast-moving pulsars

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