Near‐Infrared, Kilosecond Variability of the Wisps and Jet in the Crab Pulsar Wind Nebula

Melatos, A.; Scheltus, D.; Whiting, M. T.; Eikenberry, S. S.; Romani, Roger W.; Rigaut, François; Spitkovsky, Anatoly; Arons, Jonathan; Payne, D. J. B.

doi:10.1086/468176

Cited by 29 publications

(47 citation statements)

References 35 publications

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“…At higher magnetizations (∼ 0.1) equipartition is reached close to the TS, and most of the plasma ends in the jet. The plasma speed in the jet is in this case ∼ 0.7c, in agreement with observation of the jet in Crab Nebula and MSH 15-52 19,60,61,62 .…”

Section: Jet-torus Structure and Inner Flow Propertiessupporting

confidence: 89%

THE RELATIVISTIC WIND IN PWNe

Bucciantini

2012

Int. J. Mod. Phys. Conf. Ser.

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Pulsar Wind Nebulae (PWNe) are bubbles of relativistic plasma that form when the relativistic pulsar wind is confined by the SNR or the ISM. They have a broad band spectrum extending from from Radio to γ-rays, via synchrotron and Inverse Compton emission, and their study can provide important clues on the otherwise unobservable properties of the cold pulsar wind. The richness of emission features, revealed by recent observations, has driven a renewed interest in the theoretical modeling of these objects. In recent years an MHD paradigm has emerged. which has proved successful in explaining the richness of emission features observed in the X-ray band, and that has contributed to settle many old issues. PWNe are perhaps the best systems where relativistic dynamics can be investigated with high accuracy, given their proximity and the fact that they are persistent sources, and understanding their behavior is an essential step for the field of high energy astrophysics in general. I present here the current status of MHD models: what are the key ingredients, their successes, and open questions.

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Section: Jet-torus Structure and Inner Flow Propertiessupporting

confidence: 89%

THE RELATIVISTIC WIND IN PWNe

Bucciantini

2012

Int. J. Mod. Phys. Conf. Ser.

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“…The likely radio counterpart of the flaring component (denoted as C1) is clearly detected in this image, albeit at a somewhat smaller separation from the pulsar than the optical/X-ray emitting region Crab-A. The weak radio jet (located in the direction of the "sprite" identified in the HST images; cf., Hester et al 2002;Melatos et al 2005) and another, weaker but more compact component (C2) are also visible in the image. The possible nature of the two compact components and their relation to the flare will be discussed below.…”

Section: Image Of the Flaring Regionmentioning

confidence: 82%

VLBI imaging of a flare in the Crab nebula: more than just a spot

Lobanov

Horns

Muxlow

2011

A&A

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We report on very long baseline interferometry (VLBI) observations of the radio emission from the inner region of the Crab nebula, made at 1.6 GHz and 5 GHz after a recent high-energy flare in this object. The 5 GHz data have provided only upper limits of 0.4 milli-Jansky (mJy) on the flux density of the pulsar and 0.4 mJy/beam on the brightness of the putative flaring region. The 1.6 GHz data have enabled imaging the inner regions of the nebula on scales of up to ≈40 . The emission from the inner "wisps" is detected for the first time with VLBI observations. A likely radio counterpart (designated "C1") of the putative flaring region observed with Chandra and HST is detected in the radio image, with an estimated flux density of 0.5 ± 0.3 mJy and a size of 0 . 2-0 . 6. Another compact feature ("C2") is also detected in the VLBI image closer to the pulsar, with an estimated flux density of 0.4 ± 0.2 mJy and a size smaller than 0 . 2. Combined with the broad-band SED of the flare, the radio properties of C1 yield a lower limit of ≈0.5 mG for the magnetic field and a total minimum energy of 1.2 × 10 41 erg vested in the flare (corresponding to using about 0.2% of the pulsar spin-down power). The 1.6 GHz observations provide upper limits for the brightness (0.2 mJy/beam) and total flux density (0.4 mJy) of the optical Knot 1 located at 0 . 6 from the pulsar. The absolute position of the Crab pulsar is determined, and an estimate of the pulsar proper motion (μ α = −13.0 ± 0.2 mas/yr, μ δ = +2.9 ± 0.1 mas/yr) is obtained.

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“…1[d]), whose position and brightness vary with time in the optical, infrared and X-ray bands, and which emanate from the termination shock and move outward through the torus with inferred outflow speeds of ∼ 0.5c (Hester et al 2002, Melatos et al 2005). The exact nature of these structures is not fully understood.…”

Section: Formation Of Tori Jets and Wispsmentioning

confidence: 99%

“…In some PWNe, compact knot-like structures are observed close to the pulsar, which dissipate and reappear on timescales of order months (Hester et al 2002, Melatos et al 2005). Examples can be seen for the Crab in Figure 1(d), and similar structures are also seen for PSR B1509-58 (Gaensler et al 2002a).…”

Section: Filamentary and Compact Structures In Pwnementioning

confidence: 99%

The Evolution and Structure of Pulsar Wind Nebulae

Gaensler

Slane

2006

Annu. Rev. Astron. Astrophys.

834

809

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Pulsars steadily dissipate their rotational energy via relativistic winds.Confinement of these outflows generates luminous pulsar wind nebulae, seen across the electromagnetic spectrum in synchrotron and inverse Compton emission, and in optical emission lines when they shock the surrounding medium. These sources act as important probes of relativistic shocks, particle acceleration and of interstellar gas. We review the many recent advances in the study of pulsar wind nebulae, with particular focus on the evolutionary stages through which these objects progress as they expand into their surroundings, and on morphological structures within these nebulae which directly trace the physical processes of particle acceleration and outflow. We conclude by considering some exciting new probes of pulsar wind nebulae, including the study of TeV gamma-ray emission from these sources, and observations of pulsar winds in close binary systems.

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Near‐Infrared, Kilosecond Variability of the Wisps and Jet in the Crab Pulsar Wind Nebula

Cited by 29 publications

References 35 publications

THE RELATIVISTIC WIND IN PWNe

THE RELATIVISTIC WIND IN PWNe

VLBI imaging of a flare in the Crab nebula: more than just a spot

The Evolution and Structure of Pulsar Wind Nebulae

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