資料８－Ｈ

Commission H (Waves in Plasmas) Activity Report (ver.1)
August 31th, 2009
T. Okada, and Y. Omura

Research Topics<Akebono>
Akebono (EXOS-D) satellite has been observing electromagnetic waves in geomagnetized plasmas.
It is necessary to know the antenna impedance of the VLF electric field antennas onboard Akebono to
calibrate the electric field component data. Higashi et al. [2009] have researched the fluctuation of theantenna impedance in the short term.
In their study, a statistical analysis about the capacitance component of the antenna impedance wasdone. The capacitance components are expected to depend on the electron density because they are
determined by the thickness of the plasma sheath formed around the antenna element. However, in theanalysis of data observed by Akebono from 1989 through 1995, the effects on the capacitancecomponents of the altitude of Akebono are small (Figure 1). The effects of the strength of thegeomagnetic field and the satellite velocity are also small, and the capacitance components are almost
constant as roughly 500 pF in Akebono's orbit.
1500

Ca[pF]

1000

500

Th eoretical value ran g e

0

-500
0

2000

4000

6000

8000

10000

H[km]

Figure 1: The dependence on altitude of the capacitance component of theantenna impedance of the electric field sensors onboard Akebono.

<GEOTAIL>GEOTAIL spacecraft has been operated since 1992. The Plasma Wave Instrument (PWI) is
continuously collecting spectrum data and high time-resolution waveform data. It is expected to be in agood condition at least until the next long eclipse in 2010. The 24 hour plots of the observed wave
spectrum data have been opened in the PWI web site http://www.rish.kyoto-u.ac.jp/gtlpwi, andhttp://www.stp.isas.jaxa.jp/geotail. Furthermore, one can easily also access the PWI 2 hour plots withfull time and frequency resolution through the above web page.

1

<Cluster>
Hobara et al. (2008) have used a period of internal burst mode data from the Cluster electric field andwave instrument, who have found a number of electrostatic solitary structures in the foot region ofEarth’s quasi-perpendicular bow shock. The four individual probe potential measurements are utilized to
study the fundamental characteristics of those solitary waves; propagation vector, propagation velocity,
scale-size and potential amplitudes. Then, two classes of waves are observed; bipolar andunipolar/tripolar solitary waves. These waves are investigated in terms of BGK holes.

<BepiColombo>
The BepiColombo is the science mission to Mercury. It is the first collaborative science mission
between JAXA and ESA. The BepiColombo mission consists of two individual spacecraft called MPO(Mercury Planetary Orbiter) and MMO (Mercury Magnetospheric Orbiter). Scientists in Japan andEurope jointly proposed the plasma wave observation system called PWI (Plasma Wave Investigation).
The proposal was successfully accepted and the development of the PWI component started. The MMO
launch is scheduled in 2014. The Principal Investigator of the PWI is Prof. Yasumasa Kasaba of Tohoku
University.
The PWI investigates plasma/radio waves and DC electric field in Mercury magnetosphere. It
consists of two components of receivers, two sets of electric field sensors, two kinds of magnetic fieldsensors, and the antenna impedance measurement
system.
The PWI consists of EWO, MEFISTO-E,
SORBET, and AM2P receiver components as wellas WPT-S, MEFISTO-S as electric field sensors
and LF-SC and DB-SC as magnetic field sensors.
The engineering models of these components havebeen established and tested in Kyoto University in
April, 2009. The test results show the good features
except for non-serious problems. Furthermore, in
July, 2009, the engineering model tests with thespacecraft data handling system have been
Photo1: Engineering model of the plasma
conducted in JAXA. All of the PWI components
wave instruments onboard BepiColombo.
joined the tests and checked their function and thedigital interface with spacecraft system.

<Sounding Rocket Experiments>
S-310-38 sounding rocket experiments have been carried out at USC on 6 February, 2008. The
purpose of this experiment is the investigation of the sporadic E-region at mid latitudes. The LF/MF
band receiver (LMR) is loaded on this sounding rocket in order to measure the propagation
characteristics of LF/MF band radio waves from the ground to the lower ionosphere. The LMR measures
the received radio wave intensities from two broadcast stations at frequencies of 60 kHz and 873 kHz.
The LMR have been able to observe the relative attenuation of radio waves from ground up to theionosphere. The electron density profile in the lower ionosphere is estimated by comparing theseexperimental results with the propagation characteristics calculate by the full wave method. Figure 2
show the electron density profile and propagation characteristics of radio waves for the ascent. Leftpanel are shown electron density profile measured by the impedance probe (NEI) (blue line) andestimated by the propagation characteristics of radio waves (red line), middle panel are propagation2

characteristics of 60 kHz radio waves measured by LMR (blue line) and calculated by the full wave
method (red line), and right panel are propagation characteristics of 873 kHz radio waves. In the electron
density profile, the Es layer has a single-layer structure at the altitude of 100 km. The peak electron
density of the Es layer is 5×104 cm-3. The second peak electron density is 2×104 cm-3 at the altitude of
133 km. Then electron density profile in the lowest ionosphere at the altitude less than 90 km isestimated from radio wave propagation characteristics. The altitude profiles of radio waves are similar
for the calculated value using the estimated electron density profile and the measured value.

Figure 2: Estimation of electron density profile form the radio wave
propagation characteristics observed by S-310-38 sounding rocket.

<Polar Region Experiments>
Ozaki et al. [2009] have investigated an interesting natural harmonic VLF/LF waves observed at
Syowa station in Antarctica. The frequency components of harmonic spectrum exist in the frequency
range of 10 kHz to 100 kHz [Okada et al., 2009].
Under an assumption that the origin of the harmonic spectrum is from the magnetosphere, they havecalculated the spectrum of whistler mode waves on the ground, which are injected from themagnetosphere. The calculation results give 2 kHz and its harmonics, because the whistler mode
waves resonate in the Earth-ionosphere waveguide. However, the harmonic spectrum does not extend
over 10 kHz. Thus, the harmonic VLF/LF spectrum would not be generated inside the magnetosphere.
Also, they assumed that the origin of the harmonic spectrum is from the Earth such as sferics.
They have theoretically calculated the frequency spectrum of a sferic as shown in Figure 3. The
calculation results give the harmonic spectrum similar to the observation. Furthermore, theircalculation results show that the harmonic spectrum almost do not depend on the horizontal distance.
This suggests that the harmonic spectrum does not relate to wave propagation in the Earth-ionosphere3

waveguide. The harmonic spectrum would originate from the inherent spectrum of the sferic.

Figure 3: Calculated spectrum of a sferic propagated over a long
distance in the Earth-ionosphere waveguide.
In order to observe more events of auroral roar and Medium Frequency (MF) burst, Sato et al. (2009)
installed a receiver and loop antenna at Longyearbyen in Svalbard (CGM Lat.: 75.2 deg) in August 2008
in addition to the station at Husafell in Iceland (CGM Lat.: 65.3 deg), just in the auroral region whereauroral emissions are difficult to reach the ground due to loss in auroral ionosphere. The instrument at
Longyearbyen consists of two types of observation systems; one was designed for the continuous
observation of spectrum in a frequency range below 6 MHz. The other was designed to obtain waveform
data in a frequency range below 4 MHz, which makes it possible to determine the arrival direction of theauroral radio emissions. Some event studies suggests that MF burst is generated by high energy electrons
in lower latitude while auroral roar is generated by low energy electrons just above the station.

< KAGUYA (SELENE)>
KAGUYA (SELENE) spacecraft Lunar radar sounder (LRS) onboard the Kaguya (SELENE)
spacecraft successfully obtained 2362-hours worth of radar sounder data and 6523-hours worth ofnatural plasma wave data in the nominal operation period from October 29, 2007 to September 10, 2008
and 1714-hours worth of natural plasma wave data in the extended operation period until June 10, 2009.
Those data will contribute the sciences of the lunar geology, physics of plasma around the moon, andradio waves from the earth and other planets.
Kumamoto et al. (2009) reported that LRS observed radio waves such as auroral kilometric radiation(AKR), Type III solar radio burst, Jovian hectometric radiation (HOM), and radio communication waves
from the earth. It was found that the radio communication waves even around 5 MHz interfered withradar sounder observations when the earth’s nightside faced to the Moon. The phenomena are probably
caused by the difference of shielding effects of the earth’s ionosphere in dayside and nightside.
Nakagawa et al. (2009) made global mapping of echo power based on Lunar RadarSounder (LRS) data. It has been found that the echo power is mainly correlated with surface roughness
and also with FeO abundance in the surface determined by Lunar Prospector (LP). Correlation with FeO
abundance probably suggests the reflectivity of radio wave at the lunar surface depends not only on

4roughness but also the dielectric properties.
Lunar Ionosphere Exploration Method using Auroral Kilometric Radiation
The lunar ionosphere is known to be extremely tenuous compared with the earth's ionosphere. In
theory, the peak density is less than or equal to the solar wind density. It was, nevertheless, reported that
500-1000 cm-3 electron densities were observed at altitudes of 5-10 km with a radio occultation
technique from the Soviet Luna 19 and 22 in 1970s (Vyshlov and Savich, 1979). This report is, however,still controversial because the observed large density is difficult to explain theoretically withoutmagnetic shielding from the solar wind. So that such high densities exist, there must be unknown
maintainable or transfer mechanism of charged particles.
During the KAGUYA mission, like the Luna experiments, an electron density profile above the lunar
surface was observed by the radio occultation technique using sub-satellite (Imamura et al., 2008). Since
density of the lunar ionosphere is obtained by subtracting effects of the earth's ionosphere, estimation
accuracy of the lunar ionosphere is unfortunately restricted to that of the earth's ionosphere. On the other
hand, the KAGUYA continuously observed natural waves with the LRS-NPW and WFC instruments(Ono et al., 2008; Kasahara et al., 2008). Spectrogram of auroral kilometric radiation (AKR) whose
origin is the earth's polar region sometimes shows an interference pattern which is caused by phasedifferences between directly arrived waves and waves reflected on the lunar surface. Because plasma
frequencies of peak electron densities observed by the Luna correspond to a frequency band of the AKR
waves, the waves are reflected on the lunar ionosphere in case it exists. Goto et al. (2009) presented a
new lunar ionosphere exploration method using such interference patterns of the AKR. In this method, atheoretical interference pattern of the AKR for a given electron density profile is constructed by
calculating phase delays of reflected waves to direct waves with ray tracing. Comparing an observed
interference pattern with the theoretical ones for candidate density profiles, the most reasonable profile ischosen. This is a new approach to examine the existence of the lunar ionosphere which is not based on
the radio occultation technique. In Figure 4 as an example, they demonstrated that no dense layer existed
for an observation in the nightside region.

Figure.4: An example of interference pattern on AKR observed by LRS-NPW(2007-12-23 12:55). The horizontal axis indicates observation time (UT)
and the vertical axis does frequency in kHz. Wave intensity at eachfrequency point is given by color.

5

Lunar ULF Waves
Various magnetic fluctuations associated with the solar wind interaction with the moon were detectedby MAP-PACE/LMAG magnetometer onboard Kaguya. Most commonly observed around the moon are(1) large-amplitude, low frequency waves with the period around 100 seconds, and (2)non-monochromatic fluctuations whose frequencies range from 0.03 to 5 Hz.
The low frequency waves (0.01 Hz) detected by Kaguya, whose occurrence is often associated withthe crustal magnetic field, is supposed to be generated by the ions that are reflected by the local intensefield associated with the crustal magnetic field back into the upstream solar wind and then convected
down the solar wind stream to be detected, just like the upstream waves generated by the ions reflectedby the earth's bow shock. On the other hand, the 0.03-5 Hz fluctuations are detected by Kaguya on thesolar side surface of the moon, regardless of the crustal magnetic field. They were not observed deep inthe wake.
Such waves were also reported by Lunar Explorer as sporadic broadband (0-2Hz) magnetic
turbulence in the solar wind or wake boundary region when the spacecraft was magnetically connectedto the surface of the moon. Analogous to the whistler waves upstream of the earth's bow shock, thenon-monochromatic magnetic fluctuations are supposed to be whistler waves, mainly because of theirfrequency and the upstream propagation against the solar wind. On the other hand, it is expected that thegeneration mechanism is quite different from the monochromatic whistler waves which are often relatedwith beams of ions or electrons.

<Jupiter Observations>
By using Iitate Planetary Radio Telescope (IPRT), Tsuchiya et al. (2009) performed observation ofabsolute total flux of Jupiter’s synchrotron radiation (JSR) at several frequencies below 1 GHz, which
are not often observed by other research groups. The short-term variation of total power flux of JSR at
325 MHz shows clear correlation with the solar UV/EUV indices with a few days delay (Figure 5),
which suggest that an enhanced radial diffusion, which is driven by the neutral wind in the upper
atmosphere, is responsible for the time variation of JSR in the low frequency range.

Figure 5: Comparison between JSR observed at
325MHz and the solar EV/EUV indices from
DOY 100 to 190 in 2007.

6

Koshida et al. (2009) investigated millisecond timescale phenomena in L-burst of Jovina decametricradiation (DAM) based on the observation of Wave Form Receiver (WFR) at Iitate Planetary radio wave
observatory. New absorption phenomena with slower drift rate than that of S-burst and Fast Drift
Shadow (FDS) event, which are reported by previous studies, were found in the L-busts and named Slow
Drift Shadow (SDS) event. The analysis results suggest that these phenomena are related with Alfven
waves propagating in the Io flux tube.

<ULF Waves>
The Symposium on Electromagnetospheric Physics was held in Fukuoka, Japan, on March 4-5, 2009.
This meeting, convened by H. Kawano and K. Shiokawa, was meant as a platform where scientists
working on global observations and global simulations meet, discuss, and strengthen collaborations.
Around forty people attended, and presentations and discussions were made along the line of the global
observations and simulations, on various subjects, including ULFwaves; speakers talking on
ULF-related subjects include the following (in alphabetical order, followed by the subjects of theirtalks).
H. Kawano (MAGDAS/CPMN, ULTIMA, and ground-based remote-sensing of the magnetosphericplasma density using ULF waves), R. Nomura (Polarizations of Pc 1 pulsations observed on the groundat mid-latitudes), M. Nose ("Substorm Swift Search" website, including Wp index based on Pi 2 wave
powers), Y. Obana (Storm-time perturbations in the inner-magnetospheric plasma density,
remote-sensed from the ground using ULF waves), V. Pilipenko (Nature of Pc 3 waves above theionosphere), S. Saita (Nature of high-latitude Pc 5 waves observed by automatic ground magnetometersin Antarctica), K. Sakaguchi (Nature of EMIC waves in the inner magnetosphere, estimated from thenature of isolated proton aurorae), and M. Shinohara (Pc 5 index using low-latitude groundmagnetometers).
JPGU (Japan Geoscience Union) meeting 2009 was held in Makuhari, Japan, May 16-21, 2009.
This meeting covered a wide area of geosciences, including ULF waves, thus wide varieties of papers
were presented related to ULF waves.

<Ionospheric effects on Radio Wave Propagation>
Hayakawa et al. (2008a) have found anomalous Schumann resonance effects as observed at Moshiri(Japan) in possible association with a large earthquake (named Pingtung earthquake) (M=7.8) in Taiwan.
The anomaly is characterized by an increase in intensity at the frequencies from the 3rd to 4th resonancemodes mainly on the BEW component. Spectral modification takes place only in the UT internal of
21  1h , corresponding to the American source. This phenomenon is interpreted in terms of theinterference between the direct signal from the American lightning source and the signal scattered by theseismo-ionospheric disturbance located over Taiwan.
Hayakawa et al. (2008b) have investigated the precursory effect of ionospheric perturbations
associated with the large 2007 Niigata Chuetsu-oki earthquake by making full use of the Japanese
VLF/LF network. The ionospheric perturbation is identified from a comparison of different VLF/LF
propagation paths; JJI transmitter (Ebino, Kyushu)-Moshiri, JJY (Fukushima)-Moshiri, JJY-Kochi and
JJI-Tateyama (Chiba) and also the spatial scale of the seismo-ionospheric perturbation is estimated.
Nickolaenko et al. (2008) have compared the theoretical and experimental waveforms of ELF
transients, so-called Q bursts. The experimental data are observed with a vertical antenna in a frequency

7

range from 1Hz to 11kHz at Kochi, Japan. Experimental waveforms of several Q-bursts are comparedwith computations based on the analytical time domain solution (with the uniform Earth-ionospherecavity with a linear frequency dependence of the propagation constant). The comparison gives us goodcoincidence between the data and theory, which confirms the validity of the model and the consistencyof the source-observer distance.
Matsudo et al. (2009) have estimated the time delay of sprites behind their parent lightning discharges.
The results are summarized as follows: (i) the predominance of column sprites in winter has been
confirmed not only for the Hokuriku area but also in the Pacific Ocean, (ii)carrots are much more
frequently observed in the Pacific Ocean (with a probability of ～28％) than in the Hokuriku area (～16%), (iii) a very unique property of Hokuriku sprites is the surprisingly long delay (average ～90ms)
from their parent lightning flashes, and so on.
Myokei et al. (2009a,b) have examined the major effect in the appearance of sprites and in
determining the morphology of sprites (columns or carrots), on the basis of continuous observations of
sprites in the Hokuriku area of Japan from two sites (Chofu and Shimizu) during the three winter periods.
Detailed analysis is performed based on the estimation of the height of -10゜C at the time of sprite
occurrence. When the height of -10゜C is lower than 1800m, the occurrence of sprites is infrequent, andthe dominant shape is column. Then when it is increased (1800-3000m), a new situation takes place,
namely the occurrence of sprites is very enhanced and more spectacular shapes like carrots tend to beobserved in addition to column sprites. These informations would be of essential importance in obtaining
further understanding of generation mechanism of sprites.

<Computer simulations>
Luminous Events (like sprites)
Asano et al. (2009a) have tried to explain several unsolved questions related to transient luminous
events (like sprites) such as the long-delay and lateral shift of a sprite against its parent lightning. Theiruse of electromagnetic (EM) code of computations has shown the potential importance of the highfrequency components (like M components) in the lightning continuing current, and the simultaneouspresence of the QE (quasi-electrostatic) field and electromagnetic effect is of essential importance inaccounting for the long-delay effect of sprites. Asano et al. (2009b) have studied the effect of ahorizontal channel of the lightning stroke, which is able to explain the occasional occurrence of lateralshift of a sprite against its parent lightning.
Antenna Characteristics in Space Plasma
Suzuki et al. (2009) have investigated characteristics of the cyclotron harmonic resonances found in
the impedance probe observations in the thermal anisotropic plasma by laboratory experiment. The RF
impedance of an antenna in a thermal plasma shows resonance around the electron cyclotron harmonicfrequency. It was also found that the 2nd order of cyclotron harmonic series resonance sometimes
became much clearer than the plasma sheath resonance (Figure 6). These resonances make it difficult to
identify the upper hybrid resonance (UHR) measured by impedance probe. The results will help us tounderstand the impedance probe data affected by thermal plasma.

8

Figure 6: Variation of the probe equivalentcapacitance depending on the magnetic field
intensity. Large peaks are found at 2fc.
Hikishima et al. (2009) examined distribution functions of energetic electrons by resonant interactions
with whistler-mode rising chorus waves near the magnetospheric equator in a self-consistentelectromagnetic full-particle simulation. Figure 7 shows the time evolution of the phase space density ofenergetic electrons as a function of pitch angle in the presence of chorus emissions. The shapes of pithangle distribution are gradually deformed through a nonlinear scattering by rising chorus elements. A
large number of resonant electrons with K = 50, 100 keV are scattered inside the loss cone angle (< 20degrees). On the other hand, trapped resonant electrons are nonlinearly scattered toward higher pitch
angles. The nonlinear trappings form distribution functions of electrons with peaked at higher pitch
angles, which is called pancake distribution.
Omura et al. (2009) developed a nonlinear wave growth theory of chorus emissions, taking into
account the spatial inhomogeneity of the static magnetic field and the plasma density variation
along the magnetic field line. They derived theoretical expressions for the nonlinear growth rate andthe amplitude threshold for the generation of chorus emissions. The amplitude threshold is tested
against both observational data and self-consistent particle simulations of the chorus emissions.
They obtained equations for the wave amplitude and frequency, reproducing a rising chorus. Chorus
emissions, however, occur in two distinct frequency ranges, a lower band and an upper band,
separated at half the electron gyrofrequency. They explained the gap by means of the nonlinear
damping of the longitudinal component of a slightly oblique whistler mode wave packet
propagating along the inhomogeneous static magnetic field.

9Figure.7: Pitch angle distributions of electron phase space density withdifferent kinetic energies K = 50, 100, 200, 300 keV.

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Conferences and Meetings
1)
2)
3)
4)
5)
6)
7)
8)

Symposium on Electromagnetospheric Physics, Fukuoka, Japan, March 4-5, 2009.
3rd European Conference on Antenna and Propagation (EuCAP) 2009, Berlin March 23-27, 2009
PGU (Japan Geoscience Union) meeting 2009, Makuhari, Japan, May 16-21, 2009.
IEEE MTT-S International Microwave Symposium 2009, Boston Massachusetts June 7-12, 2009
IEEE AP-S 2009, Charleston, South Carolina May 31-June 6, 2009
International Symposium on Antenna Technology and Applied Electromagnetics (ANTEM) andthe Canadian Radio Sciences Meeting (URSI/CNC), Banff, Canada July 27-30, 2009
The 11th Scientific Assembly of IAGA, Hungary Aug. 23-30, 2009
IEEE AP-S 2010, Toronto, Ontario, Canada July 10-17, 2010

Acknowlegement
The editors thank Dr. M. Hayakawa, Dr. H. Kojima, Dr. Y. Kasahara, Dr. S.Yagitani, Dr. K.
Ishisaka, Dr. H. Kawano, Dr. A. Kumamoto and Dr. T. Nakagawa for their contribution to this report.

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