A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

Khiali, B.; Pino, E. M. de Gouveia Dal; Valle, Maŕıa Victoria del

doi:10.1093/mnras/stv248

Cited by 44 publications

(50 citation statements)

References 136 publications

(266 reference statements)

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“…Turbulent reconnection results in shrinking of 3D magnetic bundles and the charged particles entrained over magnetic loops can be accelerated by firts-order Fermi mechanism (de Gouveia dal Pino & Lazarian 2005). This mechanism has been used to model particle acceleration in several environments, including gamma-ray bursts (Zhang & Yan 2011), low luminosity AGNs (Kadowaki et al 2015), microquasars (Khiali et al 2015) and in the heliosphere (Lazarian & Desiati 2010). Interestingly, the compressibility is not necessary in this mechanism ⋆ .…”

Section: Brief Overview On Acceleration In Turbulent Reconnectionmentioning

confidence: 99%

Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission?

Brunetti¹,

Lazarían

2016

Mon. Not. R. Astron. Soc.

120

100

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In this paper we investigate a situation where relativistic particles are reaccelerated diffusing across regions of reconnection and magnetic dynamo in super-Alfvenic, incompressible large-scale turbulence. We present an exploratory study of this mechanism in the intra-cluster-medium (ICM). In view of large-scale turbulence in the ICM we adopt a reconnection scheme that is based on turbulent reconnection and MHD turbulence. In this case particles are accelerated and decelerated in a systematic way in reconnecting and magnetic-dynamo regions, respectively, and on longer time-scales undergo a stochastic process diffusing across these sites (similar to second-order Fermi). Our study extends on larger scales numerical studies that focused on the acceleration in and around turbulent reconnecting regions. We suggest that this mechanism may play a role in the reacceleration of relativistic electrons in galaxy clusters providing a new physical scenario to explain the origin of cluster-scale diffuse radio emission. Indeed differently from current turbulent reacceleration models proposed for example for radio halos this mechanism is based on the effect of large-scale incompressible and super-Alfvenic turbulence. In this new model turbulence governs the interaction between relativistic particles and magnetic field lines that diffuse, reconnect and are stretched in the turbulent ICM.

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Section: Brief Overview On Acceleration In Turbulent Reconnectionmentioning

confidence: 99%

Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission?

Brunetti¹,

Lazarían

2016

Mon. Not. R. Astron. Soc.

120

100

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“…However, on a completely different scale, the X-ray emission from the whole Solar surface shows similar behavior (Zhang 2007) where the variability is well understood to be a manifestation of magnetic reconnection process. Moreover, all accreting compact systems are believed to have magnetic fields of varying degree, making the uniqueness claim ambiguous (see, for instance, a possible magnetic reconnection scenario for flares from microquasars and non-blazar low luminous AGNs in de Gouveia dal Pino & Lazarian 2005;Kadowaki et al 2015;Khiali et al 2015;Singh et al 2015). In blazars, almost all the emission, on the other hand, is understood to be originating primarily in the jet as a result of the interaction of jet plasma and magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

Kushwaha

Sinha

Misra

et al. 2017

ApJ

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We present a statistical characterization of the γ-ray emission from the four Fermi -LAT sources: FR I radio galaxy NGC 1275, BL Lac Mrk 421, FSRQs B2 1520+31 and PKS 1510-089 detected almost continuously over a time integration of 3-days between August 2008 -October 2015. The observed flux variation is large, spanning 2 orders of magnitude between the extremes except for Mrk 421. We compute the flux distributions and compare with Gaussian and lognormal ones. We find that the 3 blazars have distribution consistent with a lognormal, suggesting that the variability is of a non-linear, multiplicative nature. This is further supported by the computation of the flux-rms relation, which is observed to be linear for the 3 blazars. However, for NGC 1275, the distribution does not seem to be represented either by a lognormal or a Gaussian, while its flux-rms relation is still found to be linear. We also compute the power spectra, which suggest the presence of a break, but are consistent with typical scale-free power-law shot noise. The results are broadly consistent with the statistical properties of the magnetic reconnection powered minijets-in-a-jet model. We discuss other possible scenarios and implications of these observations on jet processes and connections with the central engine.

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“…In a companion work we have explored the acceleration mechanism above operating in the core region of the BHBs Cyg X-1 and Cyg X-3 (see Figure 2) and have reproduced their entire observed non-thermal spectral energy distribution (SED), from the radio to the gamma-ray flux profile (see [12]). …”

Section: Discussionmentioning

confidence: 98%

The Role of Fast Magnetic Reconnection on the Radio and Gamma-Ray Emission from the Nuclear Regions of Microquasars and Low Luminosity AGNs and Black Hole Binaries and the Origin of their Gamma-Ray Emission

Kadowaki¹,

Pino²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Fast magnetic reconnection can be a very powerful mechanism operating in the core region of black hole binaries (BHBs) and active galactic nuclei (AGNs). In earlier work, we have been suggested that the power released by fast reconnection events between the magnetic field lines lifting from the inner accretion disk region and the lines anchored into the central black hole (BH) could accelerate relativistic particles in a first-order Fermi process and produce the observed radio emission from BHBs and low luminosity AGNs (LLAGNs). Moreover, we have been proposed that the observed correlation between the radio emission and the mass of these sources, spanning 10 10 orders of magnitude in mass, might be related to this process. Here we present our late results of the comparison of the magnetic power released by fast reconnection with the observed very high energy emission (from MeV/GeV to Tev bands) of BHBs, LLAGNs, blazars, and gammaray bursts (GRBs). In the case of LLAGNs and BHBs, not only the radio but also the gamma-ray emission can be due to magnetic power released by fast reconnection and follows the same trend in the luminosity-mass diagram as that of the core radio emission of these sources (tested for over 200 sources). This indicates that the very high energy emission of these sources can be produced in the core. On the other hand, the emission from blazars and GRBs does not follow the same trend, suggesting that their emission is produced outside the core, as expected. PoS(ICRC2015)919Fast Magnetic Reconnection in the Core Region of LLAGNs and BHBs Luís H. S. Kadowaki Figure 1: Schematic drawing of the magnetic field geometry in the region surrounding the BH. R X characterizes the inner accretion disk radius. ∆R X and L X correspond to the width and the extension of the magnetic reconnection region, respectively. L is the height of the corona. Obtained from [11].

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A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

Cited by 44 publications

References 136 publications

Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission?

Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission?

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

The Role of Fast Magnetic Reconnection on the Radio and Gamma-Ray Emission from the Nuclear Regions of Microquasars and Low Luminosity AGNs and Black Hole Binaries and the Origin of their Gamma-Ray Emission

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