On the role of magnetic reconnection in jet/accretion disk systems

Pino, E. M. de Gouveia Dal; Piovezan, Pamela P.; Kadowaki, L. H. S.; Kowal, Grzegorz; Lazarían, A.

doi:10.1017/s1743921310009063

Cited by 7 publications

(10 citation statements)

References 4 publications

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“…Figure 3 depicts this power as a function of the BH mass (gray region), considering a fiducial parametric space (0.0005 ≤ṁ ≤ 1, r X = 6, 1 ≤ l ≤ 18, l X ≤ l, and ψ ≃ 1) [12]. The results of this study confirmed a trend predicted earlier in [42,43] that there is a correlation between the calculated fast magnetic reconnection power and the BH mass spanning ∼ 10 orders of magnitude. This can explain not only the observed radio, but also the gamma-ray emission from GBHs and low luminous AGNs (LLAGNs).…”

Section: Pos(frapws2016)056supporting

confidence: 72%

“…[34,35]), jets and the surrounds of BHs (e.g. [16,42,43,44,45,12,19,13,30,37,38,46]), so that the information above obtained from the numerical simulations is crucial for modelling the non-thermal emission produced out of accelerated relativistic particles in such sources.…”

Section: Fast Magnetic Reconnection and Particle Accelerationmentioning

confidence: 99%

“…This model was first explored in the framework of microquasars and then extended to AGNs [42,43]. These works revealed that fast reconnection could be efficient enough to produce the core radio outbursts in microquasars and AGNs.…”

Section: Magnetic Reconnection In the Surrounds Of Bhsmentioning

confidence: 99%

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Magnetic Reconnection on Jet-Accretion Disk Systems

Pino¹,

Valle²,

Kadowaki³

et al. 2017

Proceedings of Frontier Research in Astrophysics – II — PoS(FRAPWS2016)

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Fast Magnetic Reconnection is currently regarded as an important process also beyond the solar system, specially in magnetically dominated regions of galactic and extragalactic sources like the surrounds of black holes and relativistic jets. In this lecture we discuss briefly the theory of fast magnetic reconnection, specially when driven by turbulence which is very frequent in Astrophysical flows, and its implications for relativistic particle acceleration. Then we discuss these processes in the context of the sources above, showing recent analytical and multidimensional numerical MHD studies that indicate that fast reconnection can be a powerful process to accelerate particles to relativistic velocities, produce the associated high energy non-thermal emission, and account for efficient conversion of magnetic into kinetic energy in these flows.

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Section: Pos(frapws2016)056supporting

confidence: 72%

Section: Fast Magnetic Reconnection and Particle Accelerationmentioning

confidence: 99%

See 1 more Smart Citation

Magnetic Reconnection on Jet-Accretion Disk Systems

Pino¹,

Valle²,

Kadowaki³

et al. 2017

Proceedings of Frontier Research in Astrophysics – II — PoS(FRAPWS2016)

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“…In fact, the magnetic power released in fast reconnection flares has been found to be more than sufficient to accelerate relativistic plasmons and produce the observed radio luminosity of the nuclear jets associated both to microquasars and low luminous AGNs. The observed correlation between the radio luminosity and the black hole mass in these sources, which spans 10 9 orders of magnitude in mass (Falcke et al 2004), is naturally explained in this model as simply due to the magnetic reconnection activity at the jet launching region of the accretion disk coronae of these sources (de Gouveia Dal Pino et al 2010a,2010b. A similar process may also explain the observed x-ray flares in YSOs.…”

Section: Acceleration In Agnsmentioning

confidence: 56%

“…It has been invoked in the production of ultra high energy cosmic rays (e.g. Lazarian 2000, 2001;Kotera and Olinto 2011), in jet-accretion disk systems (de Gouveia Dal Pino et al 2010a,2010bGiannios 2010;del Valle et al 2011;Ding et al 2010), and in the general framework of AGNs and GRBs (Ostrowski 2002;de Gouveia Dal Pino et al 2010a;Giannios 2010;Zhang and Yan 2011;Uzdensky 2011;Uzdensky and McKinney 2011;McKinney and Uzdensky 2012).…”

Section: Acceleration In Agnsmentioning

confidence: 99%

Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

et al. 2012

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Turbulence is ubiquitous in astrophysics. It radically changes many astrophysical phenomena, in particular, the propagation and acceleration of cosmic rays. We present the modern understanding of compressible magnetohydrodynamic (MHD) turbulence, in particular its decomposition into Alfvén, slow and fast modes, discuss the density structure of turbulent subsonic and supersonic media, as well as other relevant regimes of astrophysical turbulence. All this information is essential for understanding the energetic par- ticle acceleration that we discuss further in the review. For instance, we show how fast and slow modes accelerate energetic particles through the second order Fermi acceleration, while density fluctuations generate magnetic fields in pre-shock regions enabling the first order Fermi acceleration of high energy cosmic rays. Very importantly, however, the first order Fermi cosmic ray acceleration is also possible in sites of magnetic reconnection. In the presence of turbulence this reconnection gets fast and we present numerical evidence supporting the predictions of the Lazarian & Vishniac (1999) model of fast reconnection. The efficiency of this process suggests that magnetic reconnection can release substantial amounts of energy in short periods of time. As the particle tracing numerical simulations show that the particles can be efficiently accelerated during the reconnection, we argue that the process of magnetic reconnection may be much more important for particle acceleration than it is currently accepted. In particular, we discuss the acceleration arising from reconnection as a possible origin of the anomalous cosmic rays measured by Voyagers as well as the origin cosmic ray excess in the direction of Heliotail.

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Kinetic beaming in radiative relativistic magnetic reconnection: a mechanism for rapid gamma-ray flares in jets

Mehlhaff

Werner

Uzdensky

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Rapid gamma-ray flares pose an astrophysical puzzle, requiring mechanisms both to accelerate energetic particles and to produce fast observed variability. These dual requirements may be satisfied by collisionless relativistic magnetic reconnection. On the one hand, relativistic reconnection can energize gamma-ray emitting electrons. On the other, as previous kinetic simulations have shown, the reconnection acceleration mechanism preferentially focuses high-energy particles – and their emitted photons – into beams, which may create rapid blips in flux as they cross a telescope’s line of sight. Using a series of 2D pair-plasma particle-in-cell simulations, we explicitly demonstrate the critical role played by radiative (specifically inverse Compton) cooling in mediating the observable signatures of this ’kinetic beaming’ effect. Only in our efficiently cooled simulations do we measure kinetic beaming beyond one light crossing time of the reconnection layer. We find a correlation between the cooling strength and the photon energy range across which persistent kinetic beaming occurs: stronger cooling coincides with a wider range of beamed photon energies. We also apply our results to rapid gamma-ray flares in flat-spectrum radio quasars, suggesting that a paradigm of radiatively efficient kinetic beaming constrains relevant emission models. In particular, beaming-produced variability may be more easily realized in two-zone (e.g. spine-sheath) setups, with Compton seed photons originating in the jet itself, rather than in one-zone external Compton scenarios.

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On the role of magnetic reconnection in jet/accretion disk systems

Cited by 7 publications

References 4 publications

Magnetic Reconnection on Jet-Accretion Disk Systems

Magnetic Reconnection on Jet-Accretion Disk Systems

Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

Kinetic beaming in radiative relativistic magnetic reconnection: a mechanism for rapid gamma-ray flares in jets

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