Mechanisms for energetic particle acceleration in the solar wind

1979 ◽  
Author(s):  
L. A. Fisk
Keyword(s):  
Solar Wind ◽  
Particle Acceleration ◽  
Energetic Particle ◽  
Energetic Particle Acceleration

scholarly journals Synthesis of 3-D Coronal-Solar Wind Energetic Particle Acceleration Modules

Space Weather ◽  
2014 ◽  
Vol 12 (6) ◽  
pp. 323-328 ◽  
Author(s):  
Nathan A. Schwadron ◽  
Matt Gorby ◽  
Tibor Török ◽  
Cooper Downs ◽  
Jon Linker ◽  
...  
Keyword(s):  
Solar Wind ◽  
Particle Acceleration ◽  
Energetic Particle ◽  
Energetic Particle Acceleration

scholarly journals Fast magnetic reconnection and energetic particle acceleration

2011 ◽  
Vol 59 (7) ◽  
pp. 537-546 ◽  
Author(s):  
A. Lazarian ◽  
G. Kowal ◽  
E. Vishniac ◽  
E. de Gouveia Dal Pino
Keyword(s):  
Particle Acceleration ◽  
Magnetic Reconnection ◽  
Energetic Particle ◽  
Energetic Particle Acceleration

Energetic Particle Acceleration and Propagation in Strong CME-Less Flares

Solar Physics ◽  
2010 ◽  
Vol 263 (1-2) ◽  
pp. 185-208 ◽  
Author(s):  
K.-L. Klein ◽  
G. Trottet ◽  
A. Klassen
Keyword(s):  
Particle Acceleration ◽  
Energetic Particle ◽  
Energetic Particle Acceleration

Current sheets, magnetic islands and associated particle acceleration in the solar wind as observed by Ulysses near the ecliptic plane

2020 ◽  
Author(s):  
Olga Malandraki ◽  
Olga Khabarova ◽  
Roberto Bruno ◽  
Gary Zank ◽  
Gang Li and the ISSI-405 team
Keyword(s):  
Solar Wind ◽  
Particle Acceleration ◽  
Magnetic Reconnection ◽  
Energetic Particle ◽  
Particle Flux ◽  
Energetic Particles ◽  
Magnetic Islands ◽  
Intermittent Turbulence ◽  
Current Sheets ◽  
Energetic Particle Flux

<p>Recent studies of particle acceleration in the heliosphere have revealed a new mechanism that can locally energize particles up to several MeV/nuc. Stream-stream interactions as well as the heliospheric current sheet – stream interactions lead to formation of large magnetic cavities, bordered by strong current sheets (CSs), which in turn produce secondary CSs and dynamical small-scale magnetic islands (SMIs) of ~0.01AU or less owing to magnetic reconnection. It has been shown that particle acceleration or re-acceleration occurs via stochastic magnetic reconnection in dynamical SMIs confined inside magnetic cavities observed at 1 AU. The study links the occurrence of CSs and SMIs with characteristics of intermittent turbulence and observations of energetic particles of keV-MeV/nuc energies at ~5.3 AU. We analyze selected samples of different plasmas observed by Ulysses during a widely discussed event, which was characterized by a series of high-speed streams of various origins that interacted beyond the Earth’s orbit in January 2005. The interactions formed complex conglomerates of merged interplanetary coronal mass ejections, stream/corotating interaction regions and magnetic cavities. We study properties of turbulence and associated structures of various scales. We confirm the importance of intermittent turbulence and magnetic reconnection in modulating solar energetic particle flux and even local particle acceleration. Coherent structures, including CSs and SMIs, play a significant role in the development of secondary stochastic particle acceleration, which changes the observed energetic particle flux time-intensity profiles and increases the final energy level to which energetic particles can be accelerated in the solar wind.</p>

scholarly journals Energetic Particle Acceleration in Compressible Magnetohydrodynamic Turbulence

2021 ◽  
Vol 922 (2) ◽  
pp. 209
Author(s):  
Jian-Fu Zhang ◽  
Fu-Yuan Xiang
Keyword(s):  
Particle Acceleration ◽  
Energetic Particle ◽  
Early Stage ◽  
High Energy ◽  
Compressible Turbulence ◽  
Mode Interaction ◽  
Acceleration Of Particles ◽  
Power Law Distribution ◽  
Mhd Turbulence ◽  
Energetic Particle Acceleration

Abstract Magnetohydrodynamic (MHD) turbulence is an important agent of energetic particle acceleration. Focusing on the compressible properties of magnetic turbulence, we adopt the test particle method to study the particle acceleration from Alfvén, slow, and fast modes in four turbulence regimes that may appear in a realistic astrophysical environment. Our studies show that (1) the second-order Fermi mechanism drives the acceleration of particles in the cascade processes of three modes by particle-turbulence interactions, regardless of whether the shock wave appears; (2) not only can the power spectra of maximum-acceleration rates reveal the inertial range of compressible turbulence, but also recover the scaling and energy ratio relationship between the modes; (3) fast mode dominates the acceleration of particles, especially in the case of super-Alfvénic and supersonic turbulence, slow mode dominates the acceleration for sub-Alfvénic turbulence in the very-high-energy range, and the acceleration of Alfvén mode is significant at the early stage of the acceleration; (4) particle acceleration from three modes results in a power-law distribution in the certain range of evolution time. From the perspective of particle-wave mode interaction, this paper promotes the understanding for both the properties of turbulence and the behavior of particle acceleration, which will help provide insight into astrophysical processes involved in MHD turbulence.

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