Turbulent reconnection and its implications

Lazarían, A.; Eyink, Gregory L.; Vishniac, Ethan T.; Kowal, Grzegorz

doi:10.1098/rsta.2014.0144

Cited by 94 publications

(120 citation statements)

References 180 publications

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“…Thirdly, there is almost certainly a turbulent shear layer at the outer boundary of the jet as it transitions to the intergalactic medium. The reconnection of magnetic turbulence is also a source of high energy particles (Lazarian et al 2015). All three of these process are likely at work, repeatedly injecting new plasma at irregular intervals.…”

Section: Resultsmentioning

confidence: 99%

A Jet Source of Event Horizon Telescope Correlated Flux in M87

Punsly

2017

ApJ

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Event Horizon Telescope (EHT) observations at 230 GHz are combined with Very Long Baseline Interferometry (VLBI) observations at 86 GHz and high resolution Hubble Space Telescope optical observations in order to constrain the broadband spectrum of the emission from the base of the jet in M87. The recent VLBI observations of Hada et al provide much stricter limits on the 86 GHz luminosity and component acceleration in the jet base than was available to previous modelers. They reveal an almost hollow jet on sub-mas scales. Thus, tubular models of the jet base emanating from the innermost accretion disk are considered within the region responsible for the EHT correlated flux. There is substantial synchrotron self absorbed opacity at 86 GHz. A parametric analysis indicates that the jet dimensions and power depend strongly on the 86 GHz flux density and the black hole spin, but weakly on other parameters such as jet speed, 230 GHz flux density and optical flux. The entire power budget of the M87 jet, 10 44 ergs/sec, can be accommodated by the tubular jet. No invisible, powerful spine is required. Even though this analysis never employs the resolution of the EHT, the spectral shape implies a dimension transverse to the jet direction of 12-21 µas (∼24-27 µas) for 0.99 > a/M > 0.95 (a/M ∼ 0.7), where M is the mass and a is the angular momentum per unit mass of the central black hole.

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Section: Resultsmentioning

confidence: 99%

A Jet Source of Event Horizon Telescope Correlated Flux in M87

Punsly

2017

ApJ

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“…The interplay between these scales and the scale at which the reconnection occurs suggests cross-scale coupling with the possibility of turbulent reconnection [44][45][46]. The final article in this theme issue is a topical review by Lazarian et al [47] that discusses the topic of turbulent reconnection. In particular, through their models they show how turbulence can significantly modify reconnection, providing a mechanism for fast reconnection, and in addition violate the notion of flux freezing in collisionless plasmas.…”

Section: Synopsis Of the Issuementioning

confidence: 99%

Dissipation and heating in solar wind turbulence: from the macro to the micro and back again

Kiyani

Osman

Chapman

2015

Phil. Trans. R. Soc. A.

165

143

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The past decade has seen a flurry of research activity focused on discerning the physics of kinetic scale turbulence in high-speed astrophysical plasma flows. By ‘kinetic’ we mean spatial scales on the order of or, in particular, smaller than the ion inertial length or the ion gyro-radius—the spatial scales at which the ion and electron bulk velocities decouple and considerable change can be seen in the ion distribution functions. The motivation behind most of these studies is to find the ultimate fate of the energy cascade of plasma turbulence, and thereby the channels by which the energy in the system is dissipated. This brief Introduction motivates the case for a themed issue on this topic and introduces the topic of turbulent dissipation and heating in the solar wind. The theme issue covers the full breadth of studies: from theory and models, massive simulations of these models and observational studies from the highly rich and vast amount of data collected from scores of heliospheric space missions since the dawn of the space age. A synopsis of the theme issue is provided, where a brief description of all the contributions is discussed and how they fit together to provide an over-arching picture on the highly topical subject of dissipation and heating in turbulent collisionless plasmas in general and in the solar wind in particular.

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“…A topic intimately related to both turbulence and intermittency is that of magnetic reconnection [87][88][89][90]. In the solar wind, searches for magnetic reconnection have been less successful than in the magnetosphere, in part because the ordered large-scale magnetic field configuration prescribes the regions where the process is likely to be found.…”

Section: Evidence For Coherent Structures In the Solar Windmentioning

confidence: 99%