Theory and Applications of Non-relativistic and Relativistic Turbulent Reconnection

Lazarian, A.; Kowal, Grzegorz; Takamoto, Makoto; Pino, E. M. de Gouveia Dal; Cho, J.

doi:10.1007/978-3-319-26432-5_11

Cited by 20 publications

(15 citation statements)

References 192 publications

(284 reference statements)

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“…Kadowaki et al 2015). The turbulence could have been enhanced by feedback between the reconnections and chaotic motions of the plasma (Lazarian et al 2016). This might have led to clustering of the cells that most efficiently accelerated electrons to cause a more coherent flux outburst.…”

Section: Micro-variability In the Jetmentioning

confidence: 99%

The 2016 June Optical and Gamma-Ray Outburst and Optical Microvariability of the Blazar 3C 454.3

Weaver

Balonek

Jorstad

et al. 2019

ApJ

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The quasar 3C454.3 underwent a uniquely-structured multi-frequency outburst in June 2016. The blazar was observed in the optical R band by several ground-based telescopes in photometric and polarimetric modes, at γ-ray frequencies by the Fermi Large Area Telescope, and at 43 GHz with the Very Long Baseline Array. The maximum flux density was observed on 2016 June 24 at both optical and γ-ray frequencies, reaching S max opt = 18.91 ± 0.08 mJy and S max γ = 22.20 ± 0.18 × 10 −6 ph cm −2 s −1 , respectively. The June 2016 outburst possessed a precipitous decay at both γ-ray and optical frequencies, with the source decreasing in flux density by a factor of 4 over a 24-hour period in R band. Intraday variability was observed throughout the outburst, with flux density changes between 1 and 5 mJy over the course of a night. The precipitous decay featured statistically significant quasi-periodic micro-variability oscillations with an amplitude of ∼ 2-3% about the mean trend and a characteristic period of 36 minutes. The optical degree of polarization jumped from ∼ 3% to nearly 20% during the outburst, while the position angle varied by ∼ 120 • . A knot was ejected from the 43 GHz core on 2016 Feb 25, moving at an apparent speed v app = 20.3c ± 0.8c. From the observed minimum timescale of variability τ min opt ≈ 2 hr and derived Doppler factor δ = 22.6, we find a size of the emission region r 2.6 × 10 15 cm. If the quasi-periodic micro-variability oscillations are caused by periodic variations of the Doppler factor of emission from a turbulent vortex, we derive a rotational speed of the vortex ∼ 0.2c.

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Section: Micro-variability In the Jetmentioning

confidence: 99%

The 2016 June Optical and Gamma-Ray Outburst and Optical Microvariability of the Blazar 3C 454.3

Weaver

Balonek

Jorstad

et al. 2019

ApJ

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“…Observational testing of the theory are discussed e.g. in recent reviews by Lazarian et al (2015Lazarian et al ( , 2016.…”

Section: Introductionmentioning

confidence: 99%

Statistics of Reconnection-driven Turbulence

Kowal

Falceta‐Gonçalves

Lazarían³

et al. 2017

ApJ

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Magnetic reconnection is a process that changes magnetic field topology in highly conducting fluids. Within the standard Sweet-Parker model, this process would be too slow to explain observations (e.g. solar flares). In reality, the process must be ubiquitous as astrophysical fluids are magnetized and motions of fluid elements necessarily entail crossing of magnetic frozen in field lines and magnetic reconnection. In the presence of turbulence, the reconnection is independent of microscopic plasma properties, and may be much faster than previously thought, as proposed in and tested in Kowal et al. (2009Kowal et al. ( , 2012. However, the considered turbulence in the LazarianVishniac model was imposed externally. In this work we consider reconnection-driven magnetized turbulence in realistic three-dimensional geometry initiated by stochastic noise. We demonstrate through numerical simulations that the stochastic reconnection is able to self-generate turbulence through interactions between the reconnection outflows. We analyze the statistical properties of velocity fluctuations using power spectra and anisotropy scaling in the local reference frame, which demonstrates that the reconnection produces Kolmogorov-like turbulence, compatible with Goldreich & Sridhar (1995) model. Anisotropy statistics are, however, strongly affected by the dynamics of flows generated by reconnection process. Once the broad turbulent region is formed, the typical anisotropy scaling l ∝ l 2/3 ⊥ is formed, especially for high resolution models, were the broader range of scales is available. The decay of reconnection outflows to turbulent-like fluctuations, characterized by different anisotropy scalings, strongly depends on β plasma parameter. Moreover, the estimated reconnection rates are weakly dependent on the model resolution, suggesting that no external processes are required to make reconnection fast.

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“…It was consequently found that electrons were repeatedly accelerated at the magnetic reconnection regions within the turbulent magnetic field. Comparatively, similar works [95][96][97] presented theoretically and numerically the particle acceleration process in turbulent reconnection. An exponential growth in the energy of the accelerated particles was demonstrated along with a power law tail development in the outcome particle spectrum.…”

Section: Global Simulations With Helical Jets and Large Radiimentioning

confidence: 96%

“…On the contrary, the turbulent magnetic field-where we report multiple magnetic flux ropes-was self-consistently created in the relativistic jets, through the self-consistent disappearance/dissipation of the toroidal magnetic field. For more details, the reader is referred to similar past studies [95][96][97], where they also discussed the particle acceleration process in turbulent magnetic reconnection events, for a comparative study.…”

Section: Global Jet Simulations With a Toroidal Magnetic Field And A New Injection Schemementioning

confidence: 99%

Particle-in-Cell Simulations of Astrophysical Relativistic Jets

Meli

Nishikawa

2021

Universe

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Astrophysical relativistic jets in active galactic nuclei, gamma-ray bursts, and pulsars is the main key subject of study in the field of high-energy astrophysics, especially regarding the jet interaction with the interstellar or intergalactic environment. In this work, we review studies of particle-in-cell simulations of relativistic electron–proton (e−−p+) and electron–positron (e±) jets, and we compare simulations that we have conducted with the relativistic 3D TRISTAN-MPI code for unmagnetized and magnetized jets. We focus on how the magnetic fields affect the evolution of relativistic jets of different compositions, how the jets interact with the ambient media, how the kinetic instabilities such as the Weibel instability, the kinetic Kelvin–Helmholtz instability and the mushroom instability develop, and we discuss possible particle acceleration mechanisms at reconnection sites.

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Theory and Applications of Non-relativistic and Relativistic Turbulent Reconnection

Cited by 20 publications

References 192 publications

The 2016 June Optical and Gamma-Ray Outburst and Optical Microvariability of the Blazar 3C 454.3

The 2016 June Optical and Gamma-Ray Outburst and Optical Microvariability of the Blazar 3C 454.3

Statistics of Reconnection-driven Turbulence

Particle-in-Cell Simulations of Astrophysical Relativistic Jets

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