Modelling Jets, Tori and Flares in Pulsar Wind Nebulae

Porth, Oliver; Buehler, R.; Olmi, Barbara; Komissarov, S. S.; Lamberts, Astrid; Amato, Elena; Yuan, Yajie; Rudy, Alexander R.

doi:10.1007/s11214-017-0344-x

Cited by 38 publications

(33 citation statements)

References 169 publications

(221 reference statements)

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“…The plasma also flows to the polar region. In the presence of the magnetic hoop stress, the jets perpendicular to the torus can be formed (for a recent review on the RMHD study of PWN, please refer to Porth et al 2017).…”

Section: Summary and Discussionmentioning

confidence: 99%

Rapid X-Ray Variations of the Geminga Pulsar Wind Nebula

Hui

Lee

Kong

et al. 2017

ApJ

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A recent study by Posselt et al. (2017) reported the deepest X-ray investigation of the Geminga pulsar wind nebula (PWN) by using Chandra X-ray Observatory. In comparison with previous studies of this system, a number of new findings have been reported and we found these suggest the possible variabilities in various components of this PWN. This motivates us to carry out a dedicated search for the morphological and spectral variations of this complex nebula. We have discovered variabilities on timescales from a few days to a few months from different components of the nebula. The fastest change occurred in the circumstellar environment at a rate of 80 per cent of the speed of light. One of the most spectacular results is the wiggling of a half light-year long tail as an extension of the jet, which is significantly bent by the ram pressure. The jet wiggling occurred at a rate of about 20 per cent of the speed of light. This twisted structure can possibly be a result of a propagating torsional Alfven wave. We have also found evidence of spectral hardening along this tail for a period of about nine months.

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Section: Summary and Discussionmentioning

confidence: 99%

Rapid X-Ray Variations of the Geminga Pulsar Wind Nebula

Hui

Lee

Kong

et al. 2017

ApJ

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“…The magnetization of the pulsar wind is also comparable to ǫ B,rs in our calculation. Although this value (< 1) seems to be much smaller than that of the outflow launched initially (∼ 10 3 ), it is still within the range of magnetization at the large distance after considering the conversion of the magnetic energy to kinetic energy (seePorth et al 2017 for a review).…”

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confidence: 85%

Polarization with a Three-dimensional Mixed Magnetic Field and Its Application to GRB 170817A

Lan

Geng

et al. 2019

ApJ

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A large-scale ordered magnetic field plays a very important role in the formation and acceleration of a gamma-ray burst (GRB) jet. During the GRB prompt phase, some dissipation processes may happen and disturb the magnetic field, making the field become random to some extent. Therefore, a mixed magnetic field consisting of an ordered component and a random component is plausible for the early afterglow phase. Here we investigate the polarization evolution and light curve of an afterglow under such a 3-dimensional mixed magnetic field. Three kinds of ordered component (i.e., aligned, toroidal and radial) are discussed. We find that the three cases are distinguishable through jet polarization evolution. The polarization angle for a 3D mixed magnetic field with an aligned ordered component can evolve gradually but only changes abruptly by 90 • in the toroidal and radial cases. Furthermore, during the reverse shock crossing time, the polarization degree (PD) can be non-zero for the toroidal case but roughly zero for the radial case. Since an aligned component in a jet corresponds to a magnetar central engine and a toroidal component corresponds to a black hole, GRB central engines are distinguishable through polarization observations even if the magnetic field is mixed in a jet. In addition, our polarization calculation can be applied to GRB 170817A associated with GW170817. Using the recentlyobserved PD upper limit 12% of GRB 170817A at t = 244 days, the magnetic field strength ratio of the ordered to random components in this afterglow is constrained to be 0.9.

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“…While analysing an optical image of M87, Curtis (1918) made a note : "curious straight ray...connected with the nucleus", which was later identified and termed as 'relativistic jet' (Baade & Minkowski 1954). Since then, the observational study of jets has been revolutionized and established as ubiquitous astrophysical phenomena associated with various classes of objects like active galactic nuclei (AGN e.g., M87), young stellar objects (YSO e.g., HH 30, HH 34), X-ray binaries (e. g., SS433, Cyg X-3, GRS 1915+105, GRO 1655, Gamma ray bursts (e. g., GRB 980519), Pulsar Wind Nebulae (Porth et al 2017) etc. This paper investigates the properties of relativistic jets around black hole (hereafter BH) candidates like X-ray binaries and AGNs.…”

Section: Introductionmentioning

confidence: 99%

Radiatively driven relativistic jets in Schwarzschild space-time

Vyas

Chattopadhyay

2018

A&A

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Aims. -We carry out a general relativistic study of radiatively driven, conical fluid jets around non-rotating black holes and investigate the effects and significance of radiative acceleration, as well as radiation drag.Methods. -We apply relativistic equations of motion in curved space-time around a Schwarzschild black hole for axis-symmetric 1-D jet in steady state, plying through the radiation field of the accretion disc. Radiative moments are computed using information of curved space-time. Slopes of physical variables at the sonic points are found using L ′ Hôpital's rule and employed Runge-Kutta's 4 th order method to solve equations of motion. The analysis is carried out, using the relativistic equation of state of the jet fluid.Results. -The terminal speed of the jet depends on how much thermal energy is converted into jet momentum and how much radiation momentum is deposited on to the jet. Many classes of jet solutions with single sonic points, multiple sonic points as well as, those having radiation driven internal shocks are obtained. Variation of all flow variables along the jet-axis has been studied. Highly energetic electron-proton jets can be accelerated by intense radiation to terminal Lorentz factors γ T ∼ 3. Moderate terminal speed v T ∼ 0.5 is obtained for moderately luminous discs. Lepton dominated jets may achieve γ T ∼ 10.Conclusions. -Thermal driving of the jet itself and radiation driving by accretion disc photons produce a wide-ranging jet solutions staring from moderately strong jets to the relativistic ones. Interplay of intensity and nature of radiation field and the energetics of the jet result in such a variety in jet solutions. We show that radiation field is able to induce steady shocks in jets, one of the criteria to explain high energy power law emission observed in spectra of some of the astrophysical objects.

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Modelling Jets, Tori and Flares in Pulsar Wind Nebulae

Cited by 38 publications

References 169 publications

Rapid X-Ray Variations of the Geminga Pulsar Wind Nebula

Rapid X-Ray Variations of the Geminga Pulsar Wind Nebula

Polarization with a Three-dimensional Mixed Magnetic Field and Its Application to GRB 170817A

Radiatively driven relativistic jets in Schwarzschild space-time

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