scholarly journals Suprathermal Electron Acceleration in a Reconnecting Magnetotail: Large-Scale Kinetic Simulation

2018 ◽  
Vol 123 (10) ◽  
pp. 8087-8108 ◽  
Author(s):  
Meng Zhou ◽  
Mostafa El-Alaoui ◽  
Giovanni Lapenta ◽  
Jean Berchem ◽  
Robert L. Richard ◽  
...  
Keyword(s):  
Large Scale ◽  
Electron Acceleration ◽  
Kinetic Simulation ◽  
Suprathermal Electron

Recent scientific findings based on high-resolution core plasma imaging of the ionosphere with Swarm and ePOP

2020 ◽  
Author(s):  
David Knudsen
Keyword(s):  
High Resolution ◽  
Large Scale ◽  
Electron Acceleration ◽  
Alfven Waves ◽  
Distribution Functions ◽  
Alfvén Waves ◽  
Topside Ionosphere ◽  
High Time Resolution ◽  
Ion Heating ◽  
Suprathermal Electron

<p>The Thermal Ion Imagers on Swarm A-C, and the Suprathermal Electron/Ion Imager on ePOP (now “Swarm-E”) provide a unique view of charged particle distribution functions in the ionosphere at high time resolution (up to 100 images/s). Through high resolution, CCD-based imaging (~3000 pixels/image), ion drift velocity is derived from these images at a resolution of 20 m/s or better, and in general agreement with velocities derived from ground based radars [1] and an empirical convection model [2]. This talk reviews recent scientific applications of this technique, which are wide-ranging and include mechanisms of ion heating and upflow [3,4], M-I coupling via Alfven waves [5,6], electron acceleration and heating by Alfven waves [7,8, 9], intense plasma flows associated with “Steve” [10,11], and electrodynamics of large-scale FAC systems[ 12], among others. In addition, future opportunities made possible by these data will be discussed.</p><p>[1] Koustov et al. (2019), JGR, https://doi.org/10.1029/2018JA026245</p><p>[2] Lomidze et al. (2019), ESS, https://doi.org/10.1029/2018EA000546</p><p>[3] Shen and Knudsen (2020a), On O+ ion heating by BBELF waves at low altitude, JGR, in revision.</p><p>[4] van Irsel et al. (2020), Highly correlated ion upflow and electron temperature variations in the high latitude topside ionosphere, submitted to JGR.</p><p>[5] Pakhotin et al. (2020), JGR, https://doi.org/10.1029/2019JA027277</p><p>[6] Wu et al. (2020a), Swarm survey of Alfvenic fluctuations and their relation to nightside field-aligned current and auroral arcs systems, JGR, in revision.</p><p>[7] Liang et al. (2019), JGR, https://doi.org/10.1029/2019JA026679</p><p>[8] Wu et al. (2020b), e-POP observations of suprathermal electron bursts in the ionospheric Alfven resonator, GRL, submitted.  </p><p>[9] Shen and Knudsen (2020b), Suprathermal electron acceleration perpendicular to the magnetic field in the topside ionosphere, JGR, in press.</p><p>[10] Archer et al. (2019), JGR, https://doi.org/10.1029/2019GL082687</p><p>[11] Nishimura et al. (2019), JGR, https://doi.org/10.1029/2019GL082460</p><p>[12] Olifer et al (2020), Swarm observations of dawn/dusk asymmetries between Pedersen conductance in upward and downward FAC regions, submitted to JGR.</p><p> </p>

100-GeV large scale laser plasma electron acceleration by a multi-PW laser

2013 ◽  
Vol 11 (1) ◽  
pp. 013501-13515 ◽  
Author(s):  
Kazuhisa Nakajima Kazuhisa Nakajima ◽  
Haiyang Lu Haiyang Lu ◽  
Xueyan Zhao Xueyan Zhao ◽  
Baifei Shen Baifei Shen ◽  
Ruxin Li Ruxin Li ◽  
...  
Keyword(s):  
Laser Plasma ◽  
Large Scale ◽  
Electron Acceleration ◽  
Plasma Electron

scholarly journals VLBI for probing large-scale magnetic structures of stars

1996 ◽  
Vol 176 ◽  
pp. 173-180
Author(s):  
J.-F. Lestrade
Keyword(s):  
Magnetic Fields ◽  
Radio Emission ◽  
Large Scale ◽  
Electron Acceleration ◽  
High Gravity ◽  
Magnetic Structures

By VLBI astrometry, we show that the two RSCVn type binaries, UX Ari and σ2 CrB, have a preferred site of radio emission which is the intra-system region. It is known that radio emission from these stars is from the gyro-synchrotron process associated with large-scale magnetic fields. High gravity in the intra-system region might favor dense magnetic loops. Interactions in this region between loops attached to the surfaces of the two stellar components might produce reconnections required for electron acceleration.

scholarly journals ELECTRON ACCELERATION AT A CORONAL SHOCK PROPAGATING THROUGH A LARGE-SCALE STREAMER-LIKE MAGNETIC FIELD

2016 ◽  
Vol 821 (1) ◽  
pp. 32 ◽  
Author(s):  
Xiangliang Kong ◽  
Yao Chen ◽  
Fan Guo ◽  
Shiwei Feng ◽  
Guohui Du ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Large Scale ◽  
Electron Acceleration ◽  
Coronal Shock

Solar Wind Anomalies at 1 au and Their Associations with Large-scale Structures

2021 ◽  
Vol 923 (1) ◽  
pp. 105
Author(s):  
Yan Li ◽  
Shaosui Xu ◽  
Janet G. Luhmann ◽  
Benoit Lavraud
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Minimum ◽  
Large Scale ◽  
Spatial Scales ◽  
Radial Magnetic Field ◽  
Suprathermal Electron ◽  
Wind Structure ◽  
Solar Wind Structure ◽  
Cycle 24

Abstract We study solar wind anomalies and their associations with solar wind structures using the STEREO solar wind and suprathermal electron (STE) data from IMPACT and PLASTIC. We define solar wind anomalies as temporary and local excursions from the average solar wind state, regardless of their origins, for six anomalies: sunward strahls, counterstreaming suprathermal electrons, suprathermal electron depletions, nearly radial magnetic field episodes, anomalously low proton temperatures, and anomalously low proton beta. We first establish the solar wind synoptic contour displays, which show the expected variations in solar wind structure during the solar cycle: recurrent corotating heliospheric magnetic field (HMF) and stream structures are dominant during solar quiet times around the solar minimum (2008 December) preceding cycle 24, while complex structures characterize solar active times around the solar maximum (2014 April). During the declining phase of the cycle (2016–2019), the stream structures remain complex, but the HMF sectors show the structures of the solar minimum. We then systematically study the six anomalies by analyzing the STE data using automated procedures. All anomalies present some degree of dependence on the large-scale solar wind structure, especially around the solar minimum, implying that the solar wind structure plays a role in either the generation or transportation of these anomalies. One common feature of all of the anomalies is that the distributions of the durations of the anomalous episodes all peak at the 1 hr data resolution, but monotonically decrease over longer durations, which may arguably imply that solar anomalies occur on a continuum of temporal and spatial scales.

Suprathermal electron acceleration in the near‐Earth flow rebounce region

2017 ◽  
Vol 122 (1) ◽  
pp. 594-604 ◽  
Author(s):  
C. M. Liu ◽  
H. S. Fu ◽  
Y. Xu ◽  
T. Y. Wang ◽  
J. B. Cao ◽  
...  
Keyword(s):  
Electron Acceleration ◽  
Suprathermal Electron ◽  
Earth Flow

scholarly journals Suprathermal electron acceleration during reconnection onset in the magnetotail

2011 ◽  
Vol 29 (10) ◽  
pp. 1917-1925 ◽  
Author(s):  
A. Vaivads ◽  
A. Retinò ◽  
Yu. V. Khotyaintsev ◽  
M. André
Keyword(s):  
Magnetic Flux ◽  
Electric Field ◽  
Plasma Sheet ◽  
Electron Acceleration ◽  
Flux Transport ◽  
Energetic Electrons ◽  
Flux Tubes ◽  
Suprathermal Electron ◽  
Suprathermal Electrons ◽  
Pile Up

Abstract. We study one event of reconnection onset associated to a small substorm on 27 September 2006 by using Cluster observations at inter-spacecraft separation of about 10 000 km. We focus on the acceleration of suprathermal electrons during different stages of reconnection. We show that several distinct stages of acceleration occur: (1) moderate acceleration during reconnection of pre-existing plasma sheet flux tubes, (2) stronger acceleration during reconnection of lobe flux tubes, (3) production of the most energetic electrons within dipolarization fronts (magnetic pile-up regions). The strongest acceleration is reached at the location of Bz maxima inside the magnetic pile-up region where the reconnection jet stops. Very strong localized dawn-dusk electric field are observed within the magnetic pile-up regions and are associated to most of the magnetic flux transport.

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