The Variable Jet of the Vela Pulsar

Pavlov, G. G.; Teter, M. A.; Kargaltsev, Oleg; Sanwal, D.

doi:10.1086/375531

Cited by 176 publications

(264 citation statements)

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“…For instance, it could be a pulsar jet. Indeed, some pulsar jets are known to show extreme bending (e.g., the outer jet of the Vela pulsar; Pavlov et al 2003). The apparent lack of a similarly looking counterjet should not be surprising since the two jets can differ significantly both in shape and surface brightness due to the Doppler boost and/or proper motion effects (e.g., Pavlov et al 2003).…”

Section: Pwnmentioning

confidence: 99%

“…Indeed, some pulsar jets are known to show extreme bending (e.g., the outer jet of the Vela pulsar; Pavlov et al 2003). The apparent lack of a similarly looking counterjet should not be surprising since the two jets can differ significantly both in shape and surface brightness due to the Doppler boost and/or proper motion effects (e.g., Pavlov et al 2003). On the other hand, the ratio of the compact PWN luminosity to that of the putative jet, L pwn1 /L pwn2 ∼ 5, is noticeably larger than that in the Vela and Crab PWNe but comparable to that of the PWN around PSR B1706-44 .…”

Section: Pwnmentioning

confidence: 99%

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X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

Chang

Pavlov

Kargaltsev

et al. 2011

ApJ

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We observed the young pulsar J1357-6429 with the Chandra and XMM-Newton observatories. The pulsar spectrum fits well a combination of an absorbed power-law model (Γ = 1.7 ± 0.6) and a blackbody model (kT = 140 +60 −40 eV, R ∼ 2 km at the distance of 2.5 kpc). Strong pulsations with pulsed fraction of 42% ± 5%, apparently associated with the thermal component, were detected in 0.3-1.1 keV. Surprisingly, the pulsed fraction at higher energies, 1.1-10 keV, appears to be smaller, 23% ± 4%. The small emitting area of the thermal component either corresponds to a hotter fraction of the neutron star surface or indicates inapplicability of the simplistic blackbody description. The X-ray images also reveal a pulsar wind nebula (PWN) with complex, asymmetric morphology comprised of a brighter, compact PWN surrounded by the fainter, much more extended PWN whose spectral slopes are Γ = 1.3±0.3 and Γ = 1.7 ± 0.2, respectively. The extended PWN with the observed flux of ∼7.5 × 10 −13 erg s −1 cm −2 is a factor of 10 more luminous then the compact PWN. The pulsar and its PWN are located close to the center of the extended TeV source HESS J1356-645, which strongly suggests that the very high energy emission is powered by electrons injected by the pulsar long ago. The X-ray to TeV flux ratio, ∼0.1, is similar to those of other relic PWNe. We found no other viable candidates to power the TeV source. A region of diffuse radio emission, offset from the pulsar toward the center of the TeV source, could be synchrotron emission from the same relic PWN rather than from the supernova remnant.

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Section: Pwnmentioning

confidence: 99%

Section: Pwnmentioning

confidence: 99%

X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

Chang

Pavlov

Kargaltsev

et al. 2011

ApJ

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“…It is thought that the X-ray emission from CCOs is generally caused by the thermal cooling of the NS (e.g., Zavlin et al 1999), with typical temperatures of a few 10 6 K, as inferred from their thermal-like spectra. They have X-ray luminosities (L X ) in the range of 10 33 -10 34 erg s −1 and display X-ray spectra characterized by a black-body model with temperatures (kT ) in the range of 0.2-0.5 keV or a power-law model with very steep index Γ (see Pavlov et al 2003). Halpern & Gotthelf (2010) suggested that these objects could be weakly magnetized NSs (B ∼ 10 10 G), i.e., a kind of "anti-magnetars".…”

Section: The Nature Of Cxou J1703578-414302mentioning

confidence: 99%

“…To verify the other physical parameters of CXOU J170357.8-414302, we computed its L X and spin-down luminosityĖ, to compare with well-known CCOs objects (Pavlov et al 2003). Adopting again a mean distance of 14 kpc, we determined a total unabsorbed X-ray flux of F 0.7−2.0 = 6.9 × 10 −14 ergs cm −2 s −1 , which corresponds to an unabsorbed luminosity L X = 1.6 × 10 33 erg s −1 .…”

Section: The Nature Of Cxou J1703578-414302mentioning

confidence: 99%

An X-ray study of the SNR G344.7-0.1 and the central object CXOU J170357.8-414302

Combi

Colombo

López‐Santiago

et al. 2010

A&A

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Aims. We report results of an X-ray study of the supernova remnant (SNR) G344.7-0.1 and the point-like X-ray source located at the geometrical center of the SNR radio structure. Methods. The morphology and spectral properties of the remnant and the central X-ray point-like source were studied using data from the XMM-Newton and Chandra satellites. Archival radio data and infrared Spitzer observations at 8 and 24 µm were used to compare and study its multi-band properties at different wavelengths.Results. The XMM-Newton and Chandra observations reveal that the overall X-ray emission of G344.7-0.1 is extended and correlates very well with regions of bright radio and infrared emission. The X-ray spectrum is dominated by prominent atomic emission lines. These characteristics suggest that the X-ray emission originated in a thin thermal plasma, whose radiation is represented well by a plane-parallel shock plasma model (PSHOCK). Our study favors the scenario in which G344.7-0.1 is a 6 × 10 3 year old SNR expanding in a medium with a high density gradient and is most likely encountering a molecular cloud on the western side. In addition, we report the discovery of a soft point-like X-ray source located at the geometrical center of the radio SNR structure. The object presents some characteristics of the so-called compact central objects (CCO). However, its neutral hydrogen absorption column (N H ) is inconsistent with that of the SNR. Coincident with the position of the source, we found infrared and optical objects with typical early-K star characteristics. The X-ray source may be a foreground star or the CCO associated with the SNR. If this latter possibility were confirmed, the point-like source would be the farthest CCO detected so far and the eighth member of the new population of isolated and weakly magnetized neutron stars.

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“…For the jets in the Orion Nebula, it was also suggested that the bending may be caused by the ''rocket'' effect induced by the photoionizing UV radiation from nearby high-mass stars ; recent work by has investigated the influence of an ionizing photon flux on the jet-wind collision in the HH 555 jet. The presence of curved jets is also common to other environments, such as in active galactic nuclei, where they are observed as narrow-angleYtail radio sources (O'Dea & Owen 1986), or the pulsar jets in the Vela nebula, which are curved under the combined action of the wind within the supernova remnant and the proper motion of the pulsar (Pavlov et al 2003). Under a simplifying assumption the curvature of the jets can be described analytically (Begelman et al 1979;Canto & Raga 1995); however, these models cannot detail the shock structures and the intricate dynamics developing in the interaction and that were observed in a number of numerical studies.…”

Section: Introductionmentioning

confidence: 95%

Curved Herbig‐Haro Jets: Simulations and Experiments

Ciardi

Ampleford

Lebedev

et al. 2008

ApJ

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Herbig-Haro jets often show some degree of curvature along their path, in many cases produced by the ram pressure of a side wind. We present simulations of both laboratory and astrophysical curved jets and results from laboratory experiments. We discuss the properties and similarities of the laboratory and astrophysical flows, which show the formation of internal shocks and working surfaces. In particular, the results illustrate how the breakup of the bow shock and clumps in the flow are produced without invoking jet variability; we also discuss how jet rotation reduces the growth of the Rayleigh-Taylor instability in curved jets. Subject headingg s: ISM: Herbig-Haro objects -ISM: jets and outflows Online material: color figuresONLINE MATERIALCOLOR FIGURESFIGURE 3

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The Variable Jet of the Vela Pulsar

Cited by 176 publications

References 23 publications

X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

An X-ray study of the SNR G344.7-0.1 and the central object CXOU J170357.8-414302

Curved Herbig‐Haro Jets: Simulations and Experiments

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