COMMISSION H: Waves in Plasmas(November 2016 – October 2020)
Edited by Kojima Hirotsugu (Kyoto University, Japan), and Katoh Yuto (Tohoku
University, Japan)
1. Summary
1.1 Plasma wave observations in space and at ground stations
The most striking activity in this time period is the launch of two Japan’s spacecraft. One is theArase satellite investigating the terrestrial radiation belts and the other one is the BepiColombo
spacecraft, the mission to Mercury. The Arase satellite was launched in December 2016. The
onboard plasma wave receiver investigates wave-particle interactions that contribute to particle
scattering and accelerations (Kasaba et al., 2017a; Hikishima et al., 2018; Y. Kasahara et al., 2018;
Katoh et al., 2018a; Kumamoto et al., 2018; Matsuda et al., 2018b; Miyoshi et al., 2018a, 2018b;
Ozaki et al., 2018c). The launch of the BepiColombo was in December 2018. The mission isdesigned under the collaboration of ESA and JAXA. The onboard plasma wave receiver proceeds
the first observation of plasma waves in Mercury (Kasaba et al., 2020a).
The BepiColombo will arrive at Mercury in 2025, while the Arase has got its extensive
observations started in March 2017. One of the crucial targets in the Arase mission is to investigate
the nonlinear interactions of electrons and whistler mode chorus emissions. S. Kasahara et al. (2018)
demonstrated that the Arase satellite found the direct evidence of the pitch angle scattering by
whistler mode chorus waves. The satellite clearly showed the flux modulations inside the loss conethat are correlated with the lower-band chorus bursts. Both the flux modulations and the chorus
bursts have a good correlation with the pulsating aurora. Kurita et al. (2018a) found the deformationof electron pitch angle distributions associated with upper band chorus emissions. They showed tensof keV electrons were accelerated by upper-band chorus within 30 seconds. Another target of the
Arase mission is the ElectroMagnetic Ion Cyclotron (EMIC) wave. Matsuda et al. (2018a)
statistically showed the spatial distribution of EMIC waves depending on their types. Shoji et al.
(2018) demonstrated that the observed EMIC waves with rising or falling frequencies agree with thenonlinear theory. In the further low frequency bands, Nose et al. (2018) found strong magnetic field
fluctuations in the frequency close to the local gyrofrequency of O+ ions with the depolarization
signatures in the deep inner magnetosphere.
The unique feature of the Arase satellite is that its designed orbits allow us to coordinate
collaborative observations with other satellites and ground stations. Kurita et al. (2018b) found rapid
loss of relativistic electrons by EMIC waves in the outer radiation belt observed by Arase, Van Allen
Probes, and the PWING ground stations during the geomagnetic storm on March 21, 2017,1

associated with an arrival of CIR in the solar wind. Ozaki et al. (2019) succeeded a visualization ofwave–particle interactions by the coordinated observations of chorus waveforms by the Arasesatellite and transient auroral flashes from electron precipitation observed by a ground-based
EMCCD camera of the PWING project. Miyoshi et al. (2019) revealed EMIC waves converted fromequatorial noise due to M/Q=2 ions in the plasmasphere based on observations from Van Allen
Probes and Arase satellites. Hosokawa et al. (2020) reported the first direct correspondence between
the main/internal modulations of the pulsating aurora and chorus burst of rising tone elements fromsimultaneous satellite-ground based observations.
The Hisaki satellite has been continuing the mission to observe planets. Kimura et al. (2018)
investigated the response of Jupiter’s aurora to mass loading from Io with a newly developed modeland data from the Hisaki satellite. They found that during volcanic eruptions at Io, impulsive
variation of aurora responded to the mass loading rate rather than the solar wind.
The space around the moon has been studied under the cooperative observations by the Kaguya
and Geotail spacecraft. Nakagawa et al. (2018) found the narrow band EMIC waves on the lunar
orbit in the Earth’s magnetotail. They discussed the generation mechanism and showed the cyclotron
resonance with anisotropic ions in the plasma sheet.
1.2 Development of new plasma wave instruments and observation techniques
The effort to miniaturizations of plasma wave receivers and sensors have been made to meet limited
resources for micro-satellite missions in future. Ozaki et al. (2016) and Zushi et al. (2019) succeeded
in developing the small sensor preamplifier and small spectrum receiver by designing analog chips
through the development of the ASIC (Application Specific Integrated Circuits).
The Wave-Particle Interaction Analyzer (WPIA) is the new method in the direct measurement ofwave-particle interaction, which is implemented in the Arase satellite. Kitahara and Katoh (2016)devised the new method for the direct detection of pitch angle scattering by extending the WPIA.
Shoji et al. (2017) applied the WPIA method to THEMIS data and succeeded in identifying
quantitative wave-particle interactions on the observed EMIC waves. The result clearly indicatedthat the rising tone of EMIC waves are caused by non-linear wave-particle interactions with ring
current ions.
Neural network is applied to a large amount of observation data. Santosa and Hobara (2017)
Nighttime VLF amplitude transmitted from Hawaii in the path to Japan is predicted by using
Nonlinear Autoregressive with Exogenous Input Neural Network (NARX NN) model.
1.3 Computer simulations, modeling and theories on plasma waves
Wave-particle interactions between energetic electrons and whistler-mode chorus have been
intensively studied. Hsieh and Omura (2017) revealed the contribution of nonlinear wave trapping2

by obliquely propagating whistler-mode waves on the relativistic electron acceleration. Kubota andOmura (2018) developed a new numerical Green's function method originally proposed by Omura etal. (2015) for the nonlinear dynamics of radiation belt electrons interacting with chorus emissions
and reproduced the rapid formation of radiation belt electron fluxes by chorus emissions propagating
parallel to the dipole geomagnetic field line. Hsieh et al. (2020) applied the numerical Green's
function method to obliquely propagating chorus emissions and showed that oblique chorus
energizes keV electrons to about 2 MeV rapidly within several emissions. Omura et al. (2019)confirmed the efficient acceleration of relativistic electrons at Landau resonance with obliquely
propagating whistler-mode chorus emissions by theory, simulation, and observation. Kitahara andKatoh (2019) studied the mechanism of anomalous trapping at low pitch angles caused by coherent
whistler-mode waves and examined its contribution on energetic electron precipitation to theatmosphere. Katoh and Omura (2016) carried out simulation of whistler-mode chorus generation
with real parameters in the Earth's inner magnetosphere and reproduced spectral fine structures as
observed by the Cluster spacecraft (Santolik et al., 2003; Santolik, 2008). Katoh et al. (2018b)
revealed the dependence of chorus generation process on the temperature anisotropy and density ofenergetic electrons by a series of self-consistent electron hybrid code simulations.
Wave-particle interactions around a collisionless shock have been actively studied by full particle
simulations. Otsuka et al. (2019) performed a one-dimensional full particle-in-cell (PIC) simulationof a quasi-parallel collisionless shock with the Alfvén Mach number 6.6 and a shock angle of 20
degrees to investigate the interactions between self-consistently produced backstreaming ions andupstream waves. Matsukiyo et al. (2020) solved a shock tube problem by one-dimensional fullparticle-in-cell simulations under the condition that a relatively tenuous and weakly magnetizedplasma is continuously pushed by a relatively dense and strongly magnetized plasma having
supersonic relative velocity. The results are discussed in the context of the heliospheric boundary
region or heliopause. Umeda et al. (2019) conducted a numerical experiment for laboratory
experiments on the generation of magnetized collisionless shocks with high-power lasers by using
one-dimensional particle-in-cell simulation.
Darian et al. (2019) studied the effect of an external magnetic field on the formation of the wakein the potential distribution behind a dust grain with self-consistent Particle-In-Cell numericalsimulations. The topology of the wake field is significantly affected by the magnetization degree ofplasma and by the ion flow speed. The external magnetic field acts to reduce the potential
enhancements in the wake and leads to the splitting of the wake pattern.
Usui et al. (2019) and Miyake et al. (2020) investigated the plasma-spacecraft interactions byusing the PIC simulations. Usui et al. (2019) found the existence of a distorted plasma depetion
region in a satellite wake, while Miyake et al. (2020) identified wing-like density structures formedby electrons reflected at a negatively-charged moving spacecraft in a magnetized plasma. Such3

structures are characterized by the trail of field-aligned propagation of Langmuir waves. Reflected
electrons cause spurious electric fields that can be measured by double probes on a satellite.

2. Activity Report

Status of projects related with plasma wave observation
1.

BepiColombo/MMO
http://global.jaxa.jp/projects/sat/bepi/
http://www.stp.isas.jaxa.jp/mercury/p_mmo.html
BepiColombo is a Mercury exploration project jointly planned by JAXA and the European
Space Agency (ESA). It consists of two orbiters; the Mercury Planetary Orbiter (MPO) and the
Mercury Magnetosphere Orbiter (MMO). JAXA is responsible for development of the MMO.
MMO is at ESA/ESTEC (European Space Research and Technology Centre, Netherlands) from
April 2015. For the plasma wave, Plasma Wave Investigation(PWI) (PI: Y. Kasaba [Tohoku
Univ.]) is aboard this spacecraft. PWI will first observe electric field, plasma waves, and radio
waves around Mercury, which were not covered by past spacecraft. The spacecraft was
successfully launched om Oct. 2018 from Kourou (Arival at the Mercury in 2025). The PWI
science team has shiftted to develop the telemetry data pipelines and operation planning for thereal science execution which will be realized in 2020s. The spacecraft will experience flybys
before the arrival of the Mercury. The first Venus flyby has succeeded in Oct. 2020.

2.

JUICE
http://www.isas.jaxa.jp/en/missions/spacecraft/future/juice.html
JUICE (JUpiter ICy moons Explorer) is the L-class mission of ESA, planned for launch in 2022
and arrival at Jupiter in 2029. It will spend at least three years making detailed observations of
the Jovian system including Ganymede, Calisto and Europa, and finally be on the orbit around
Ganymede. For the plasma wave, Radio and Plasma Wave Investigation (PI: J.-E. Wahlund[IRF Uppsala, Sweden]) is aboard this spacecraft and covers the information of the exospheres,
surfaces, and conducting subsurface oceans of icy satellites and their interactions withsurrounding Jovian magnetosphere. For the access to the conductive subsurface ocean, RPWI
will first observe cold plasma and electric fields, to separate the global conductivity and current
from the ionospheres. As a byproduct, reflected Jovian radio emission can be expected from theboundary of crust (ice) and subsurface ocean (conductive water). From Japan, High Frequency
part (RWI-Preamp and HF-Receiver) will be supplied (Co-PI: Y. Kasaba [Tohoku Univ.]) andprovide the highly resolved information of Jovian radiation emitted from Jupiter and Ganymedeby the first 3-axis E-field measurement. Our Flight Models was tested in Europe (Kasaba et al.,2016; Katoh et al., 2017; Kumamoto et al., 2017).

3.

Arase (ERG)
http://www.isas.jaxa.jp/en/missions/spacecraft/current/erg.html
4http://ergsc.isee.nagoya-u.ac.jp/index.shtml.en
The Arase (ERG; Exploration of energization and Radiation in Geospace) project is a mission
to study acceleration and loss mechanisms of relativistic electrons around the Earth. The Arase(ERG) was launched in Dec., 2016, and the prime mission started in March, 2017. The Plasma
Wave Experiment (PWE, PI: Y. Kasahara [Kanazawa Univ.]) has measured DC electric fieldand plasma waves in the inner magnetosphere covering wide frequency range from DC to 10
MHz for electric field and from a few Hz to 100 kHz for magnetic field. The Software-Wave
Particle Interaction Analyzer (SWPIA) (PI: H. Kojima, [Kyoto. Univ.]) is equipped to realize
direct measurements of interactions between energetic electrons and whistler-mode chorus in
the Earth's inner magnetosphere.
Varieties of wave phenomena such as chorus, EMIC, ULF pulsations and lightning whistlers
have been successfully observed by the PWE. We have also conducted cooperative observations
with the ground-based stations, Van Allen Probes and the other satellites in the magnetosphere.
We intensively conducted the PWE burst mode operations, by which waveforms were
continuously captured. During the prime mission, all science instruments have operated in good
health and the JAXA has approved the mission extension of Arase until end of March,2022(Kasaba et al., 2017a; Hikishima et al., 2018; Y. Kasahara et al., 2018; Katoh et al., 2018a;
Kumamoto et al., 2018; Matsuda et al., 2018b; Miyoshi et al., 2018a, 2018b; Ozaki et al.,2018c).

4.

Hisaki spacecraft
http://www.isas.jaxa.jp/en/missions/spacecraft/current/hisaki.html
Hisaki satellite with the EUV spectrometer (Extreme Ultraviolet Spectroscope for Exospheric
Dynamics: EXCEED) is the UV/EUV space telescope dedicated to planetary sciences.
Hisaki has provided continuous observations of Jovian system in UV aurora total flux and EUV
Io torus plasma distributions and plasma diagnostics, which connected the solar windinformation and ground-based radio (Decameter [aurora] - VHF [radiation belt]) and IR (aurora
and airglows) observations. From July 2016, NASA Juno orbiter started the observation around
Jupiter. Hisaki’s priority is on the support observation for this mission. The Hisaki mission
period has extended until the end of Mar. 2022.

5.

GEOTAIL
http://www.isas.jaxa.jp/en/missions/spacecraft/current/geotail.html
GEOTAIL spacecraft has been operated since 1992. The Plasma Wave Instrument (PWI) is
continuously collecting the high resolution waveform data as well as the spectrum data. The
color plots of the observed wave spectrum data have been opened in the PWI web site
http://space.rish.kyoto-u.ac.jp/gtlpwi, and http://www.stp.isas.jaxa.jp/geotail. One can easily
also make the color spectrum plots in flexible time scales at https://geotail.nict.go.jp/.
56.

Iceland - Syowa conjugate observation
A new VLF instrument has been installed at Husafell observatory in Iceland in
September, 2016. Unique conjugate observations of auroral phenomena including
the measurements of ULF and VLF waves have been carried out between Icelandand Syowa Station, Antarctica since 1983 by the National Institute of Polar
Research in Japan in collaboration with University of Iceland.

7.

Ground-based observation of solar and planetary radio waves
http://pparc.gp.tohoku.ac.jp/research/iprt
http://ariel.gp.tohoku.ac.jp/jupiter/
Ground-based observation of solar and planetary radio waves is performed using IPRT (Iitate
Planetary Radio Telescope) and HF antenna array developed by Tohoku University. IPRT has
been operated at the Iitate observatory in Fukushima Japan since 2000. IPRT measures meter todecimeter natural radio waves at fixed frequencies of 325 and 785 MHz using LNA and also
from 150 to 500 MHz using wide-band receiver. Primary purposes of the telescope are toinvestigate the dynamic behavior of Jupiter's synchrotron radiation and solar radio emissions in
the low-frequency range. In addition to this, IPRT has capability to observe weak radio sourcesin the low frequency range such as pulsars. HF antenna at Iitate observatory has been operated
since 1996 for ground-based observation of Jovian decametric radiation (DAM; 15-40MHz).
Wide-band spectrum monitor, and waveform receiver with single antenna, and long-baseline
interferometer with 3 station's antenna (Kawatabi, Zao, and Yoneyama) are in operation. For
observation of weaker non-Io Jovian DAM events, short-baseline interferometer with fourantennas is also operated.

8.

PWING Project
http://www.isee.nagoya-u.ac.jp/dimr/PWING/en/
The PWING project investigates the process of dynamical variation of the particles and waves
in the Earth’s inner magnetosphere and clarify the mechanism of the dynamical variation
quantitatively. This project has operated eight ground-based stations separately positioned in thelongitudinal direction at subauroral latitudes in Canada, Alaska, Russia, Finland, and Iceland,
using induction magnetometers, riometers, VLF/ELF receivers, and all-sky airglow/aurora
imagers and EMCCD cameras since March 2017. Conjugate measurements of particles andwaves with the new ERG (Arase) satellite and the Van Allen Probes has been made extensively
in 2017-2020. The budget for PWING will be finished in March 2021. But the ground-based
observation will be continued as possible as we can (Shiokawa et al., 2017).

9.

Bilateral project between JSPS and CAS
This is the joint project between JSPS and CAS (PI: Y. Miyoshi/O. Santolik) for plasma waves
as well as lightnings using multi-satellite and ground-based data. The project will be finished in
6March 2021.

10. HpFP protocol
http://hpfp.nict.go.jp/
Due to rapid increase of network bandwidth, applications and systems working in long fat
network (LFN) play more important roles. For effective development of them, precise
measurements of network conditions are significant. Transmission Control Protocol (TCP) is
the most commonly used protocol, but is essentially unable to achieve high throughput in LFNs
with packet losses. For this reason, it is hard for conventional network measurement tools toshow the maximum or available bandwidth in LFN, especially in high packet loss environments.
To overcome this issue, we introduced a novel data transfer protocol on TCP/IP transport layer,
namely high-performance and flexible protocol (HpFP). For high-precision pace control andretransmission control, the HpFP intermittently monitors network conditions such as packet loss
and latency. We develop an application via the HpFP, named hperf, which measures end-to-end
throughput as well as status of packet loss and latency in LFNs. We carried out experiments to
examine the abilities of the hperf in high-throughput data transfer and measurement of network
qualities in terms of packet loss and latency(Figure 1). The hperf achieves almost wire-rate
throughput, 10 Gbps, on the international link between Japan and the USA with even 0.5\%
packet loss ratio (PLR). The measurements of packet loss and latency show goodcorrespondence with the conventional methods via iperf and ping. These results are verified in
our laboratory experiments on 10 Gbps link using a network simulator as well. We conclude
that the HpFP has significant potential for a variety of network applications and the hperf is agood network quality measurement tool in LFNs, compared to the conventional TCPs.

Figure1: Laboratory experiment result of HpFP and TCP on LNF.

11. Development of Real-Time Monitoring System via Visual IoT
Visual Internet of Things (IoT) is a class of IoT that collects rich visual data. In general, the7visual IoT device is equipped with a video transmission equipment such as a camera. The
involved technologies are advanced video transmission techniques and information extraction
from images by image recognition techniques. However, since the video data size is larger than
the sensor data size, one of the issues of visual IoT is high-performance video transmission in
networks in which the bandwidths are limited. In this project[2017], we designed anddeveloped a real-time monitoring system using visual IoT device. Our system is based on anovel protocol, named high-performance video transmission (HpVT), for field monitoring via
4G LTE mobile networks(Figure 2). The performance of our system is evaluated in real fields toconclude that we can achieve full high-definition (full-HD) resolution video transmission withas high frame rate as 30 fps.

Figure 2: A schematic concept of Visual IoT.

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