Effective Proton Heating through Collisionless Driven Reconnection in the Presence of Guide Field

Usami, Shunsuke; Horiuchi, Ritoku; Ohtani, Hiroaki; Ono, Yasushi; Tanabe, Hiroshi

doi:10.1585/pfr.13.3401025

Cited by 6 publications

(13 citation statements)

References 11 publications

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“…As Refs. [12] and [13] demonstrated, ringshaped velocity distributions are formed, which means that the velocity distributions are expanded and ions are effectively heated in the downstream.…”

Section: Particle Simulation Methods and Resultsmentioning

confidence: 97%

“…This simulation run is the same as a run which has been performed in Refs. [12,13]. Figure 1 (a) shows the spatial profile of the ion temperature perpendicular to the local magnetic field as color contours and the magnetic field lines at ω pi t = 775.…”

Section: Particle Simulation Methods and Resultsmentioning

confidence: 99%

“…The separatrix width is quite thin for ions. Hence, ions behave as nonadiabatic upon crossing the separatrix [7,12,13]. In the basic theory, when ions enter the downstream across the separatrix, their entry speed is suf- ficiently small so that we regard it as zero for the ideal case.…”

Section: Basic Theorymentioning

confidence: 99%

“…The solid lines denote a typical EX-ion, and the dashed lines represent a BS-ion, which was introduced in Ref. [13], for comparison. Figure 5 (a) shows the orbits of the ion particles, where the color contours indicate the electric field E y .…”

Section: Test Particle Simulationmentioning

confidence: 99%

“…One can derive where plasma particles are accelerated or heated and what mechanism acts for the plasma acceleration and heating by analyzing velocity distribution. In preceding simulation works by Usami et al [12,13], on author's e-mail: usami.shunsuke@nifs.ac.jp * ) This article is based on the presentation at the 27th International Toki Conference (ITC27) & the 13th Asia Pacific Plasma Theory Conference (APPTC2018).…”

Section: Introductionmentioning

confidence: 99%

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Horn-Shaped Structure Attached to the Ring-Shaped Ion Velocity Distribution during Magnetic Reconnection with a Guide Field

Usami

Horiuchi

Ohtani

2019

Plasma and Fusion Research

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The characteristic feature of a "horn-shaped velocity distribution" in magnetic reconnection in the presence of a guide field is investigated by means of simulation and theory. Particle simulations show that a horn-shaped velocity structure is formed in the downstream, concomitant with a ring-shaped velocity distribution studied in the preceding works. The theory which explains the motion of ions responsible for the horn-shaped structure is constructed as an extension of the basic theory for the ring-shaped structure. In the extended theory, ions are accelerated in the inflow direction by an electrostatic field in the separatrix, and thus the gyration speed of such ions in the downstream is larger than that for the basic theory. Test particle simulations confirm that some ions behave as in the extended theory and form the horn-shaped velocity structure.

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Section: Particle Simulation Methods and Resultsmentioning

confidence: 97%

Section: Particle Simulation Methods and Resultsmentioning

confidence: 99%

Section: Basic Theorymentioning

confidence: 99%

Section: Test Particle Simulationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Horn-Shaped Structure Attached to the Ring-Shaped Ion Velocity Distribution during Magnetic Reconnection with a Guide Field

Usami

Horiuchi

Ohtani

2019

Plasma and Fusion Research

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Multi-scale simulations of particle acceleration in astrophysical systems

Marcowith

Ferrand

Grech

et al. 2020

Living Rev Comput Astrophys

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This review aims at providing an up-to-date status and a general introduction to the subject of the numerical study of energetic particle acceleration and transport in turbulent astrophysical flows. The subject is also complemented by a short overview of recent progresses obtained in the domain of laser plasma experiments. We review the main physical processes at the heart of the production of a non-thermal distribution in both Newtonian and relativistic astrophysical flows, namely the first and second order Fermi acceleration processes. We also discuss shock drift and surfing acceleration, two processes important in the context of particle injection in shock acceleration. We analyze with some details the particle-in-cell (PIC) approach used to describe particle kinetics. We review the main results obtained with PIC simulations in the recent years concerning particle acceleration at shocks and in reconnection events. The review discusses the solution of Fokker–Planck problems with application to the study of particle acceleration at shocks but also in hot coronal plasmas surrounding compact objects. We continue by considering large scale physics. We describe recent developments in magnetohydrodynamic (MHD) simulations. We give a special emphasis on the way energetic particle dynamics can be coupled to MHD solutions either using a multi-fluid calculation or directly coupling kinetic and fluid calculations. This aspect is mandatory to investigate the acceleration of particles in the deep relativistic regimes to explain the highest cosmic ray energies.

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Energy transfer and electron energization in collisionless magnetic reconnection for different guide-field intensities

Pucci

Usami

et al. 2018

Physics of Plasmas

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Electron dynamics and energization are one of the key components of magnetic field dissipation in collisionless reconnection. In 2D numerical simulations of magnetic reconnection, the main mechanism that limits the current density and provides an effective dissipation is most probably the electron pressure tensor term, that has been shown to break the frozen-in condition at the x-point. In addition, the electron-meanderingorbit scale controls the width of the electron dissipation region, where the electron temperature has been observed to increase both in recent Magnetospheric Multiple-Scale (MMS) observations as well as in laboratory experiments, such as the Magnetic Reconnection Experiment (MRX). By means of two-dimensional fullparticle simulations in an open system, we investigate how the energy conversion and particle energization depend on the guide field intensity. We study the energy transfer from magnetic field to the plasma in the vicinity of the x-point and close downstream regions, E·J and the threshold guide field separating two regimes where either the parallel component, E || J || , or the perpendicular component, E ⊥ · J ⊥ , dominate the energy transfer, confirming recent MRX results and also consistent with MMS observations. We calculate the energy partition between fields, kinetic, and thermal energy of different species, from electron to ion scales, showing there is no significant variation for different guide field configurations. Finally we study possible mechanisms for electron perpendicular heating by examining electron distribution functions and self-consistently evolved particle orbits in high guide field configurations.

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Effective Proton Heating through Collisionless Driven Reconnection in the Presence of Guide Field

Cited by 6 publications

References 11 publications

Horn-Shaped Structure Attached to the Ring-Shaped Ion Velocity Distribution during Magnetic Reconnection with a Guide Field

Horn-Shaped Structure Attached to the Ring-Shaped Ion Velocity Distribution during Magnetic Reconnection with a Guide Field

Multi-scale simulations of particle acceleration in astrophysical systems

Energy transfer and electron energization in collisionless magnetic reconnection for different guide-field intensities

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