Pulsar Wind Nebulae

Mitchell, Alison; Gelfand, Joseph D.

doi:10.1007/978-981-16-4544-0_157-1

Cited by 4 publications

(3 citation statements)

References 183 publications

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“…For our dynamical one-zone scenario of the PWN, we have eight parameters: where ν c increases with time as nearly t 2 . Hereafter we assume n 0,2 to be 1, to be consistent with r - 1 cm m 3 ej p in the following time evolution according to Mitchell & Gelfand (2022). For observational constraints, we obtain t 2 = 0.0027 by applying ν c = 5.5 GHz.…”

Section: Parameter Constraints and Resultsmentioning

confidence: 99%

A Generic Model for a Persistent Radio Source around Fast Radio Bursts

Chen,

Tong

2024

ApJ

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The repeated fast radio bursts FRB 121102A and FRB 190520B have been reported, along with a spatially coincident, compact, persistent radio emission. In this paper, we present a parameterized one-zone model, with the basic scenario that a relativistic magnetized wind from the pulsar sweeps up the surroundings, e.g., freely expanding supernova ejecta, giving rise to a power-law distribution of electrons between the forward shock and the termination shock. We show that via appropriate adjustment of the model parameters, we can obtain synchrotron radio emission properties from the one-zone model bright enough to account for the observation, simply and analytically fitting the observed spectra well. Through dynamical evolution of the model, we can also obtain time-varying relevant properties. This parameterized model does not depend on concrete physical models such as a central engine; instead, we can constraint the physical model via comparison between parameters and observations, indicating the information about the central engine and surroundings. We also discuss the synchrotron self-Compton emission in our scenario in the end but find no clue about the counterparts at other wave bands.

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Section: Parameter Constraints and Resultsmentioning

confidence: 99%

A Generic Model for a Persistent Radio Source around Fast Radio Bursts

Chen,

Tong

2024

ApJ

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“…However, unlike thermal emission, synchrotron radiation in PWNe is linearly polarised, with the degree of polarisation ranging from a few per cent to more than 30% (e.g. Mitchell & Gelfand, 2022). Typically, the magnetic field within PWNe is assumed to be toroidal (van der Swaluw, 2003;Porth et al, 2017).…”

Section: Polarisation Analysismentioning

confidence: 99%

Fast as Potoroo: Radio continuum detection of a bow-shock pulsar wind nebula powered by pulsar J1638–4713

Lazarević,

Filipović,

Dai

et al. 2024

Publ. Astron. Soc. Aust.

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We report the discovery of a bow-shock pulsar wind nebula (PWN), named Potoroo, and the detection of a young pulsar J1638–4713 that powers the nebula. We present a radio continuum study of the PWN based on 20-cm observations obtained from the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. PSR J1638–4713 was identified using Parkes radio telescope observations at frequencies above 3 GHz. The pulsar has the second-highest dispersion measure of all known radio pulsars (1553 pc cm–3), a spin period of 65.74 ms and a spin-down luminosity of Ė = 6.1 × 1036 erg s–1. The PWN has a cometary morphology and one of the greatest projected lengths among all the observed pulsar radio tails, measuring over 21 pc for an assumed distance of 10 kpc. The remarkably long tail and atypically steep radio spectral index are attributed to the interplay of a supernova reverse shock and the PWN. The originating supernova remnant is not known so far. We estimated the pulsar kick velocity to be in the range of 1000 – 2000 km s–1 for ages between 23 and 10 kyr. The X-ray counterpart found in Chandra data, CXOU J163802.6–471358, shows the same tail morphology as the radio source but is shorter by a factor of 10. The peak of the X-ray emission is offset from the peak of the radio total intensity (Stokes I) emission by approximately 4.7”, but coincides well with circularly polarised (Stokes V) emission. No infrared counterpart was found.

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“…PWN continuum emission can typically be described with PL models over broad wavelength ranges (e.g., Mitchell & Gelfand 2022). The slope of the continuum spectrum can vary spatially across the PWN, and the canonical PWN model of fainter outer regions emitting softer spectra stems from the idea of synchrotron cooling.…”

Section: Spatial Variations Of the Spectral Index Within The Pulsar W...mentioning

confidence: 99%

Spatial Variations and Breaks in the Optical–Near-infrared Spectra of the Pulsar and Pulsar Wind Nebula in Supernova Remnant 0540–69.3

Tenhu,

Larsson,

Sollerman

et al. 2024

ApJ

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The supernova remnant (SNR) 0540–69.3, twin of the Crab Nebula, offers an excellent opportunity to study the continuum emission from a young pulsar and pulsar wind nebula (PWN). We present observations taken with the Very Large Telescope instruments MUSE and X-shooter in the wavelength range 3000–25000 Å, which allow us to study spatial variations of the optical spectra, along with the first near-infrared (NIR) spectrum of the source. We model the optical spectra with a power law (PL) F ν ∝ ν −α and find clear spatial variations (including a torus–jet structure) in the spectral index across the PWN. Generally, we find spectral hardening toward the outer parts, from α ∼ 1.1 to ∼0.1, which may indicate particle reacceleration by the PWN shock at the inner edge of the ejecta or alternatively time variability of the pulsar wind. The optical–NIR spectrum of the PWN is best described by a broken PL, confirming that several breaks are needed to model the full spectral energy distribution of the PWN, and suggesting the presence of more than one particle population. Finally, subtracting the PWN contribution from the pulsar spectrum we find that the spectrum is best described with a broken-PL model with a flat and a positive spectral index, in contrast to the Crab pulsar that has a negative spectral index and no break in the optical. This might imply that pulsar differences propagate to the PWN spectra.

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Pulsar Wind Nebulae

Cited by 4 publications

References 183 publications

A Generic Model for a Persistent Radio Source around Fast Radio Bursts

A Generic Model for a Persistent Radio Source around Fast Radio Bursts

Fast as Potoroo: Radio continuum detection of a bow-shock pulsar wind nebula powered by pulsar J1638–4713

Spatial Variations and Breaks in the Optical–Near-infrared Spectra of the Pulsar and Pulsar Wind Nebula in Supernova Remnant 0540–69.3

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