Particle acceleration and transport by strong MHD-turbulence and shock wave ensembles

1992 ◽  
Author(s):  
A. M. Bykov
Keyword(s):  
Shock Wave ◽  
Particle Acceleration ◽  
Mhd Turbulence

TRANSPORT EQUATION FOR MHD TURBULENCE: APPLICATION TO PARTICLE ACCELERATION AT INTERPLANETARY SHOCKS

2009 ◽  
Vol 696 (1) ◽  
pp. 261-267 ◽  
Author(s):  
Igor V. Sokolov ◽  
Ilia I. Roussev ◽  
Marina Skender ◽  
Tamas I. Gombosi ◽  
Arcadi V. Usmanov
Keyword(s):  
Particle Acceleration ◽  
Transport Equation ◽  
Interplanetary Shocks ◽  
Mhd Turbulence

scholarly journals The Interaction of Current Sheets with a Shock Wave and Particle Acceleration

2020 ◽  
Vol 1620 ◽  
pp. 012014
Author(s):  
Masaru Nakanotani ◽  
Gary P. Zank ◽  
Lingling Zhao
Keyword(s):  
Shock Wave ◽  
Particle Acceleration ◽  
Current Sheets

scholarly journals Particle Acceleration in the Heliosphere

1995 ◽  
Vol 10 ◽  
pp. 307-309
Author(s):  
Loukas Vlahos
Keyword(s):  
Particle Acceleration ◽  
Energy Dissipation ◽  
Electric Field ◽  
Solar Surface ◽  
Interplanetary Medium ◽  
Acceleration Process ◽  
Mhd Turbulence ◽  
Dissipation Process ◽  
Planetary Magnetospheres ◽  
Dissipation Processes

The heliosphere could be divided in three major acceleration Laboratories, the solar surface (Laboratory 1), the interplanetary medium (Laboratory 2) and Earth and Planetary magnetospheres (Laboratory 3). Our understanding of the acceleration process depends strongly on the nature of the drivers and the energy dissipation process. The energy gain by a particle with velocity where is the variation of the electric field in space and time. All three Laboratories mentioned above share a common characteristic, the drivers and the energy dissipation processes are closely connected to fully developed MHD turbulence. We can show that our understanding of particle acceleration depends strongly on the interaction of particles with fields resulting from fully developed MHD turbulence.

scholarly journals Particle Acceleration in the Process of Eruptive Opening and Reconnection of Magnetic Fields

1980 ◽  
Vol 91 ◽  
pp. 217-221 ◽  
Author(s):  
Z. Švestka ◽  
S. F. Martin ◽  
R. A. Kopp
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Particle Acceleration ◽  
Magnetic Fields ◽  
Magnetic Loop ◽  
Coronal Loops ◽  
X Rays ◽  
Flare Loops ◽  
Field Lines ◽  
The Magnetic Field

In a series of papers on the flare of 29 July 1973 (Nolte et al., 1979; Martin, 1979; Švestka et al., 1979) it has been shown that Hα “post-flare” loops are the cooled aftermath of previously hot coronal loops which were visible in x-rays in the same position earlier in the flare. Kopp and Pneuman (1976) have proposed that these post-flare loops are formed by a process of successive magnetic field reconnections of previously distended magnetic field lines as illustrated in Figure 1. Each successive reconnection of the magnetic field yields a closed magnetic loop that forms above and concentric with previously formed loops. A shock wave created during each sudden reconnection travels down both legs of each loop and provides energy for ionizing chromospheric mass at the footpoints of the loop. Subsequent condensation of the ionized mass at the tops of the loops renders them visible as this mass falls to the chromosphere.

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.

scholarly journals Models of particle acceleration in galaxy clusters by MHD turbulence

2009 ◽  
Vol 5 (H15) ◽  
pp. 466-467
Author(s):  
G. Brunetti
Keyword(s):  
Particle Acceleration ◽  
Radio Emission ◽  
Galaxy Clusters ◽  
Indirect Evidence ◽  
Mhd Turbulence ◽  
Radio Data ◽  
Central Cluster ◽  
Relativistic Particles

AbstractPresent radio data provide indirect evidence that diffuse radio emission in the central cluster regions may originate from turbulent-acceleration of relativistic particles. I was invited to discuss models of particle acceleration by MHD turbulence in clusters and in these pages I briefly touch the main points of my talk.

scholarly journals Particle Acceleration and Radio Emission of the Supernovae Remnants at Different Stages of their Evolution

1983 ◽  
Vol 101 ◽  
pp. 183-186
Author(s):  
V. N. Fedorenko
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Particle Acceleration ◽  
Radio Emission ◽  
Temporal Evolution ◽  
Relativistic Electrons ◽  
List Type ◽  
Type Number ◽  
Physical Processes ◽  
The Magnetic Field

In this Paper, I consider physical processes, governing relativistic electrons in SNRs. a)SNRs at the age t > 102 yr. I argue that the shock wave acceleration faces some difficulties. Then I show that the temporal evolution of the SNRs radio emission can be accounted for without involving the acceleration.b)SNRs at the age t < 102 yr. I associate the lack of radio emission at this stage (Brown and Marscher, 1978) with the weakness of the magnetic field.c)I infer that the most efficient particle acceleration and radio emission of the SNRs should occur at the stage t ~ 102 yr.

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