Particle acceleration in self-driven turbulent reconnection

Zhang, Jian-Fu; Xu, Siyao; Lazarian, Alex; Kowal, Grzegorz

doi:10.1016/j.jheap.2023.08.001

Cited by 4 publications

(3 citation statements)

References 93 publications

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“…Our reconnection simulations demonstrated that particles within and around the turbulent reconnection layer can be accelerated up to relativistic energies (Liang et al 2023;Zhang et al 2023). The interactions of accelerated particles with turbulent magnetic fields would emit synchrotron signals, which can reveal the information of magnetic turbulence.…”

Section: Generation Of Polarization Observational Datamentioning

confidence: 84%

“…Numerical attempts demonstrated the generation of turbulence by reconnection itself in both cases of the incompressible (Beresnyak 2017) and compressible MHD (Oishi et al 2015;Huang & Bhattacharjee 2016;Kowal et al 2017;Liang et al 2023). Recently, our numerical studies also demonstrated that charged particles can be effectively accelerated in reconnection-driven turbulence by test particle simulations (Zhang et al 2023) and MHD-PIC methods (Liang et al 2023).…”

Section: Introductionmentioning

confidence: 82%

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Studying Magnetic Reconnection with Synchrotron Polarization Statistics

Zhang,

Liang,

Xiao

2024

ApJ

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Magnetic reconnection is a fundamental process for releasing magnetic energy in space physics and astrophysics. At present, the usual way to investigate the reconnection process is through analytical studies or first-principle numerical simulations. This paper is the first to understand the turbulent magnetic reconnection process by exploring the nature of magnetic turbulence. From the perspective of radio synchrotron polarization statistics, we study how to recover the properties of the turbulent magnetic field by considering the line of sight along different directions of the reconnection layer. We find that polarization intensity statistics can reveal the spectral properties of reconnection turbulence. This work opens up a new way of understanding turbulent magnetic reconnection.

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Section: Generation Of Polarization Observational Datamentioning

confidence: 84%

Section: Introductionmentioning

confidence: 82%

Studying Magnetic Reconnection with Synchrotron Polarization Statistics

Zhang,

Liang,

Xiao

2024

ApJ

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“…5 Compared to the results from different integrators, we obtained consistent results with that of the RK4 method. See footnote 4 in Zhang et al (2023) for more details. magnetic field, B, it is not difficult to understand the behavior of the particles' motion.…”

Section: Trajectory Of Particlesmentioning

confidence: 99%

The Diffusion and Scattering of Accelerating Particles in Compressible MHD Turbulence

Gao,

Zhang

2024

ApJ

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We numerically study the diffusion and scattering of cosmic rays (CRs) together with their acceleration processes in the framework of the modern understanding of magnetohydrodynamic (MHD) turbulence. Based on the properties of compressible MHD turbulence obtained from observations and numerical experiments, we investigate the interaction of CRs with plasma modes. We find that (1) the gyroradius of particles exponentially increases with the acceleration timescale; (2) the momentum diffusion presents the power-law relationship with the gyroradius in the strong turbulence regime, and shows a plateau in the weak turbulence regime implying a stochastic acceleration process; (3) the spatial diffusion is dominated by the parallel diffusion in the sub-Alfvénic regime, while it is dominated by the perpendicular diffusion in the super-Alfvénic one; (4) as for the interaction of CRs with plasma modes, the particle acceleration is dominated by the fast mode in the high β case, while in the low β case, it is dominated by the fast and slow modes; and (5) in the presence of acceleration, magnetosonic modes still play a critical role in the diffusion and scattering processes of CRs, which is in good agreement with earlier theoretical predictions.

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Velocity gradient and stellar polarization: magnetic field tomography towards the L1688 cloud

Schmaltz,

Hu,

Lazarian

2024

Monthly Notices of the Royal Astronomical Society

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Magnetic fields are a defining yet enigmatic aspect of the interstellar medium (ISM), with their three-dimensional mapping posing a substantial challenge. In this study, we harness the innovative Velocity Gradient Technique (VGT), underpinned by magnetohydrodynamic (MHD) turbulence theories, to elucidate the magnetic field structure by applying it to the atomic neutral hydrogen (HI) emission line and the molecular tracer 12CO. We construct the tomography of the magnetic field in the low-mass star-forming region L1688, utilizing two approaches: (1) VGT-HI combined with the Galactic rotational curve, and (2) stellar polarization paired with precise star parallax measurements. Our analysis reveals that the magnetic field orientations deduced from stellar polarization undergo a distinct directional change in the vicinity of L1688, providing evidence that the misalignment between VGT-HI and stellar polarization stems from the influence of the molecular cloud’s magnetic field on the polarization of starlight. When comparing VGT-12CO to stellar polarization and Planck polarization data, we observe that VGT-12CO effectively reconciles the misalignment noted with VGT-HI, showing statistical alignment with Planck polarization measurements. This indicates that VGT-12CO could be integrated with VGT-HI, offering vital insights into the magnetic fields of molecular clouds, thereby enhancing the accuracy of our 3D magnetic field reconstructions.

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Particle acceleration in self-driven turbulent reconnection

Cited by 4 publications

References 93 publications

Studying Magnetic Reconnection with Synchrotron Polarization Statistics

Studying Magnetic Reconnection with Synchrotron Polarization Statistics

The Diffusion and Scattering of Accelerating Particles in Compressible MHD Turbulence

Velocity gradient and stellar polarization: magnetic field tomography towards the L1688 cloud

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