PEM09-01

日本地球惑星科学連合2016年大会

赤道MUレーダー計画の現状２０１６
Status of Equatorial MU Radar project in 2016*山本 衛1、橋口 浩之1、津田 敏隆1*Mamoru Yamamoto1, Hiroyuki Hashiguchi1, Toshitaka Tsuda1
1.京都大学生存圏研究所
1.Research Institute for Sustainable Humanosphere, Kyoto University
Research Institute for Sustainable Humanosphere, Kyoto University (RISH) has been studying theatmosphere and ionosphere by using radars. The first big facility was the MU (Middle and Upper
atmosphere) radar installed in Shiga, Japan in 1984. This is one of the most powerful andmulti-functional radar, and is successful of revealing importance of atmospheric waves for the
dynamical vertical coupling processes. The next big radar was the Equatorial Atmosphere Radar (EAR)
installed at Kototabang, West Sumatra, Indonesia in 2001. The EAR was operated under close
collaboration with LAPAN (Indonesia National Institute for Aeronautics and Space), and conducted
the long-term continuous observations of the equatorial atmosphere/ionosphere. The EAR, however,
had a limited sensitivity to the MU radar as the total output power is just 1/10 to the MU radar.
Our new project is to establish "Equatorial MU Radar (EMU)" just next to the EAR site in Indonesia.
The EMU will have an active phased array antenna with the 163 m diameter and 1055 cross-element
Yagis. Total output power of the EMU will be more than 500 kW. The EMU is the "MU radar class"facility, and can detect turbulent echoes from the mesosphere (60-80 km). In the ionosphereincoherent-scatter observations of plasma density, drift, and temperature would be possible.
Multi-channel receivers will realizes radar-imaging observations. The EMU is one of the key elementin the project "Study of coupling processes in the solar-terrestrial system" that is one of theimportant project in the Master Plan 2014 of the Science Council of Japan (SCJ). In 2015 the MU
radar was awarded IEEE Milestone as the world first atmospheric radar with active phased array
antenna system. For the EAR, preparation for construcion permission has almost completed. We willreport current status of the EMU project together with stutus of the Master Plan 2017 of SCJ.
キーワード：大気レーダー、赤道大気、低緯度電離圏、インドネシア
Keywords: Atmospheric radar, Equatorial atmosphere, Low-latitude ionosphere, Indonesia©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-01 -PEM09-02

日本地球惑星科学連合2016年大会

NASA Ionospheric Connection Explorer, Validation of Scientific Performance*Thomas J Immel1, Scott England1, Ellen Taylor1, Stephen Mende1, Jerry Edelstein1, Eric Korpela1,
Harald Frey1, Roderick Heelis2, Russell Stoneback2, Christoph Englert3, Kenneth Marr3, Jonathan
Makela4, Brian Harding4, Farzad Kamalabadi4, Dimitrious Iliou4
1.University of California, Berkeley, 2.University of Texas at Dallas, 3.Naval Research Laboratory,
4.University of Illinois
Earth's space environment is highly variable, changing in ways that we are currently unable topredict. Specifically, the ionosphere exhibits remarkable day-to-day changes that cannot be
attributed to any known source, though forcing from the lower atmosphere is now considered of key
importance. NASA's Ionospheric Connection Explorer, a mission designed to discover the causes ofthis variability, is in development for a June 2017 launch. Concurrent with the build of the
instruments and spacecraft, a science validation effort has tracked the expected performance of theobservatory. The predicted performance of the science retrieval algorithms developed for ICON will
be reported. The current performance models show that ICON will have outstanding scientificcapability and be able to address and resolve the open questions in space plasma physics thatpertain to space weather. Here we will present the performance predictions and observational plans
for the ICON mission, and discuss opportunities for collaborative measurements aligned withinternational research efforts.
Keywords: Thermosphere, Ionosphere, atmospheric physics©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-02 -PEM09-02©2016. Japan Geoscience Union. All Right Reserved.

日本地球惑星科学連合2016年大会- PEM09-02 -PEM09-03

日本地球惑星科学連合2016年大会

Pre-YMC2015キャンペーン速報
Early Results from pre-YMC 2015 Field Campaign in Sumatra*米山 邦夫1、鈴木 順子1、城岡 竜一1、森 修一1、勝俣 昌己2、Syamsudin Fadli3、Nurhayati Noer4*Kunio Yoneyama1, Junko Suzuki1, Ryuichi Shirooka1, Shuichi Mori1, Masaki Katsumata2, Fadli
Syamsudin3, Noer Nurhayati4
1.海洋研究開発機構 基幹研究領域 大気海洋相互作用研究分野、2.海洋研究開発機構

地球環境観測研究開発センター、3.インドネシア技術評価応用庁、4.インドネシア気象気候地球物理庁
1.Japan Agency for Marine-Earth Science and Technology / Department of Coupled
Ocean-Atmosphere-Land Processes Research, 2.Research and Development Center for Global Change,
3.Agency for the Assessment and Application of Technology, 4.Agency for Meteorology Climatology andGeophysics
The Years of the Maritime Continent (YMC) is designed to take place from mid-2017 to mid-2019 for
improving our understanding and prediction of the weather-climate system over the Maritime
Continent (MC) region and its global impact. During the campaign period, several intensive
observations coordinated under the framework of YMC are planned in addition to the long-termmonitoring by the MC local agencies. However, such coordination and conducting observations may
encounter unforeseen difficulties. In addition, 2-year period is still insufficient to understandeven local-scale phenomena as it may be affected by large/longer-scale phenomena such as El Nino.
By considering these factors, we have conducted another field campaign as a pilot study for the
YMC, and we call it as pre-YMC campaign. This campaign was conducted in Sumatra, Indonesia
including Bengkulu (on and off the coast) and Kototabang from November through December 2015. While
we deployed land-based radar/special radiosonde sites in Bengkulu and the R/V Mirai off Bengkulu to
study precipitation mechanism, we also conducted water vapor/ozone-sonde observations at the EAR
site in Kototabang to study upper troposphere/stratosphere interactions. Observations captured theatmospheric features in the transition phase from inactive to active for convection associated with
the Madden-Julian oscillation. In this talk, some selected early results will be presented inaddition to the basic information about the field campaign.
キーワード：国際集中観測YMC、集中観測Pre-YMC、スマトラ島
Keywords: YMC, Pre-YMC, Sumatra©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-03 -PEM09-04

日本地球惑星科学連合2016年大会

Cloud Propagation over Sumatera during Coupling Processes in the Equatorial Atmosphere
Campaign I and II*Marzuki Marzuki1, Aulya Rahayu1, Mutya Vonnisa1, Hiroyuki Hashiguchi2
1.Department of Physics, Andalas University, 2.Research Institute for Sustainable Humanosphere(RISH), Kyoto University
Cloud propagation determines the distribution of precipitation. Previous studies on cloudpropagation over Sumatera are mostly focused on mean propagation. Marzuki et al. [1] investigatedthe propagation of individual cloud cluster using Hovmoller diagram of 10 years of brightness
temperature data. However, cloud tracking through Hovmoller diagram has some disadvantages: 1)
result significantly depends on the averaging window, 2) two or more cloud can be assumed as asingle cloud if they lie at the same longitude at the same time, and 3) only possible to get one
direction of propagation. Therefore, objectively identifying and tracking the cloud inlatitude-longitude space is necessary. In this study, we present the result of cloud tracking basedon three-dimensional brightness temperature (Tb) data during Coupling Processes in the Equatorial
Atmosphere (CPEA) campaign I and II. The two campaigns have a different Madden-Julian Oscillation(MJO) phase in which active MJO was observed during the CPEA-I in contrast to the CPEA-II. Althoughduring the CPEA-II strong actively convective due to the MJO was not observed, Sumatra received
high daily rainfall during this period. Although mean outgoing longwave radiation (OLR) is much
lower during CPEA-II than CPEA-I, the cloud size during the CPEA-I is larger than during CPEA-II.
It was also found that the ratio of westward to eastward moving cloud during CPEA-I (II) is 7:1(6:1). Both during CPEA-I and II, westward moving streaks generally have a longer span and faster
speed than those of eastward-moving system.
[1] Marzuki, Hashiguchi, H., Yamamoto, M. K., Yamamoto, M., Mori, S., Yamanaka, M. D., Carbone, R.
E., and Tuttle, J. D.: Cloud episode propagation over the Indonesian Maritime Continent from 10
years of infrared brightness temperature observations, Atmos. Res., 120–121, 268–286, 2013.
Keywords: Cloud propagation, Sumatra, CPEA-I and II©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-04 -PEM09-05

日本地球惑星科学連合2016年大会

Coordinated observations of post-midnight irregularities and thermospheric neutral wind
and temperature*Tam Dao1, Yuichi Otsuka1, Kazuo Shiokawa1, Michi Nishioka2, Mamoru Yamamoto3, Suhaila M. Buhari 4
1.Institute for Space-Earth Environmental Research, Graduate school of Science, Nagoya University,
Nagoya, japan., 2.National Institute of Information and Communication Technology, Tokyo, Japan,
3.Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Japan., 4.Universiti
Teknologi Malaysia, Malaysia
Field-aligned irregularities (FAIs) have been observed since last few decades by using UHF/VHF/HF
radars. At equatorial F-region, FAIs are generated within plasma bubbles. The plasma bubbles are
well-known to be initiated at evening terminator and occur frequently in equinoxes, especiallyduring high solar activity conditions. On the other hand, recent observations show that the FAIs
frequently occur at post-midnight around June solstice in low solar activity conditions. From thecomparison of ionosonde data, it is found that uplift of the F layer could play an important rolein generating the post-midnight plasma bubbles. However, mechanisms of uplift of the F layer has
not been revealed yet.
In this study, we investigate an event of the post-midnight FAIs observed with the EAR (Equatorial
Atmospheric Radar) at Kototabang in Indonesia. Two-dimensional map of rate of total electron
content change index (ROTI) obtained from GPS receivers in Southeast Asia, thermospheric neutral
winds and temperature observed at Kototabang by Fabri-Perot interferometer, and altitude of thebottomside of the F layer observed with ionosondes at Kototabang, Chumphon, and Chiang Mai, arecompared. On the night of July 9, 2010, the post-midnight FAIs appeared within the field of view of
the EAR. By estimating the vertical rise velocity of this FAI structure, we found that the FAIs
could be accompanied by plasma bubble initiated at magnetic equator around 22:00 LT.
Two-dimensional ROTI map also showed an enhancement near magnetic equator around this time, thenextended to the higher low latitudes and reached Kototabang at midnight. Thermospheric neutral wind
was southward (magnetically poleward) from19:30 to 23:00 LT, and northward (magneticallyequatorward) enhancement was observed from 22:30 LT. The altitude of the bottomside of F-layer
increased at 15:30-16:00 LT. This altitude increase of the F layer could be caused by theenhancement of the equatorward thermospheric wind. Thermospheric neutral temperature was higher at
north than at south from 22:30 to 01:00 LT on the subsequent day, indicating that Midnight
Temperature Maximum (MTM) existed at the north of Kototabang. We discuss a role of MTM in thegeneration of post-midnight FAIs at low latitude region.
Keywords: Post-midnight F layer field-aligned irregularities (FAIs) , Plasma bubbles, Equatorial
Ionospheric region©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-05 -PEM09-06

日本地球惑星科学連合2016年大会

Coordinated Incoherent Scatter Radar and Fabry-Perot Interformeter observations ofionosphere-thermosphere
disturbances during the March 17-18, 2015 great solar storm*Shunrong Zhang1, Phil Erickson1, Anthea Coster1, Mike Sulzer2, Michael Nicolls2, Mary McCready2,
Yuichi Otsuka3, Jonathan Makela4, John Noto5
1.Massachusetts Institute of Technology, 2.SRI International, 3.Nagoya University, 4.University of
Illinois at Urbana-Champaign, 5.Scientific Solution, Inc.
With a tremendous drop of the Dst index to ~ -230 nT, the geomagnetic storm during March 17-18,
2015 has been the largest during the current solar cycle. This strom was caused by a combined
effect of the arriving solar Coronal Mass Ejection materials with high-speed solar wind streams
originated from a nearby coronal hole. It was very fortunate for us to have coordinated aninternational campaign monitoring geospace disturbances during this period using ground-based
facilities. These include incoherent scatter radars and Fabry-Perot Interferometers in the America
sectors and other instruments in East Asia sectors, forming an observational network along
approximately the 60W/120E meridional circle. The presentation will highlight these ground-based
observations along with simultaneous DMSP in situ measurements and TEC from a network of dense GPS
receivers, with a focuses on (1) the ion-neutral coupling processes at subauroral andmid-latitudes; (2) periodic midlatitude ionospheric disturbances; and (3) topside ionosphericvariations. In particular, one of the most striking features to be discussed is the unexpected
pre-midnight northward neutral wind surge, observed over multiple subauroral and midlatitude sites,
accompanying strong westward winds developed at earlier times. We ascribe these wind disturbances
to Subauroal Polarization Stream (SAPS).
Keywords: geomagnetic storm, magnetosphere-ionosphere-thermosphere coupling, incoherent scatterradar, Fabry-Perot Interformeter©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-06 -PEM09-07

日本地球惑星科学連合2016年大会

地球大気を制御する赤道域の海岸線
Equatorial coastlines controlling Earth's atmosphere*山中 大学1*Manabu D. Yamanaka1
1.海洋研究開発機構大気海洋相互作用研究分野
1.Department of Coupled Ocean-Atmosphere-Land Processes Research, Japan Agency for Marine-Earth
Science and Technology
Just half a century has passed since the theories of vertically evanescent tides (Kato, 1966) andequatorially ducting modes (Matsuno, 1966) as varieties of atmospheric gravity waves. Horizontal
convections as superimpositions of upward/downward gravity waves are generated between dayside andnightside hemispheres and between land and sea surfaces by insolation with diurnal cycles.
Importance of the latter category, so-called sea-land breeze circulation, has been emphasized byground-based and space-borne observations over the equatorial troposphere. The cloud activity has
diurnal and annual cycles dominantly on land, in contrast to intraseasonal and interannual
variations mainly over oceans, and the tropical rainfall amount is expressed by functions ofcoastal distance and length (Ogino et al., 2016; Yamanaka, 2016). This explains the global cloud
activity-rainfall maximum located over the Indonesian maritime continent (IMC) with the world’s
longest coastlines.
The diurnal cycle is generated directly by land-sea temperature contrast along a coastline: solid
land becomes hotter than liquid sea by solar heating through clear sky before noontime, andopposite contrast appears before the sunrise by evening rainfall-induced sprinkler-like landcooling in tropics (different from infrared cooling at clear night in extratropics). This is why
the diurnal cycle is dominant in the rainy season, and also why the rainy season appears exactly inthe summer-side hemisphere, because land heating in the clear morning and water-vapor transport byafternoon sea-wind are strongest in the season of maximum insolation. El Niño causes less rainfall,because lower sea surface temperature makes morning maritime convection weaker.
Those lower-atmospheric features are reflected in the middle- and upper atmospheric dynamics. As
suggested so far (e.g., Ogino et al., 1995; Tsuda et al., 2000), the stratospheric gravity-wave
activity takes maximum near the equator and in particular near IMC as does the convective activity.
Here it is suggested from the latter that these activities are generated with diurnal cycles andhorizontal scales of about 300 km along coastlines, which are fixed with the major islands and thewhole IMC with zonal scales of 1,000 and 5,000 km, respectively. 14-year hourly 25 km-resolution
cloud-top height data are analyzed to show spectral slopes of around -2 for frequency and -5/3 and-3 for higher and lower zonal wavenumbers (with a border of about 300 km in zonal wavelength), as
have shown already for tropopausal gravity waves or quasi-two dimensional turbulence (e.g., Nastrom
and Gage, 1985). A part of the insolation over equatorial lands sequentially with Earth’s rotation
may contribute (through infrared absorption) to generation of migrating tides. All the features
mentioned here appear on a land-sea coexistent planet like Earth, and differences in other planets
are also discussed briefly.
キーワード：赤道域、大気・海洋・陸面相互作用、地球自転・公転
Keywords: equatorial region, air-sea-land interaction, Earth's rotation and revolution©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-07 -PEM09-07©2016. Japan Geoscience Union. All Right Reserved.

日本地球惑星科学連合2016年大会- PEM09-07 -PEM09-08

日本地球惑星科学連合2016年大会

太陽地球系結合過程の研究のための名古屋大学宇宙地球環境研究所の地上ネットワーク観測
Ground network observation of ISEE, Nagoya University, for the study of coupling processes
in solar-terrestrial system*塩川 和夫1、大塚 雄一1、檜山 哲哉1、西谷 望1、三好 由純1、草野 完也1*Kazuo Shiokawa1, Yuichi Otsuka1, Tetsuya Hiyama1, Nozomu Nishitani1, Yoshizumi Miyoshi1, Kanya
Kusano1
1.名古屋大学宇宙地球環境研究所
1.Institute for Space-Earth Environmental Research, Nagoya University
The Solar-Terrestrial Environment Laboratory, Nagoya University has been combined with Hydrospheric
Atmospheric Research Center and Center for Chronological Research to become the Institute forSpace-Earth Environment Research (ISEE) of Nagoya University since October 2015. Under the new
institution, ground-based observation network has been kept operating to study coupling processes
in solar-terrestrial system, particularly at ground stations in Asia and Africa from high to low
latitudes. A new collaborative research system will be launched from April 2016 particularly toextend this ground network observations in collaboration with various Japanese and foreign
institutions. The Center for International Collaborative Research (CICR) and Center for Integrated
Data Science (CIDAS) are newly established under ISEE to promote international collaborative
researches and to promote integrated analyses using various kinds of observation data and advanced
computer simulations, respectively. These centers also contribute to the operation and database
construction of the ground-based network observation by ISEE. In this presentation, we show
ground-based network observations and domestic and international collaboration system newly
developed under ISEE and its two centers.
キーワード：地上ネットワーク観測、宇宙地球環境研究所、共同利用・共同研究
Keywords: Ground network observation , Institute for Space-Earth Environment Research (ISEE),
Nagoya University, cooperative research©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-08 -PEM09-09

日本地球惑星科学連合2016年大会

MAGDASプロジェクトの進展：国際協力の戦略
Recent development of MAGDAS project: Strategy for international alliance of geomagnetic
field network observation
吉川 顕正1,2、*阿部 修司2、魚住 禎司2、藤本 晶子2、松下 拓輝3、河野 英昭1,2
Akimasa Yoshikawa1,2, *Shuji Abe2, Teiji Uozumi2, Akiko Fujimoto2, Hiroki Matsushita3, Hideaki Kawano
1,2

1.九州大学大学院理学研究院地球惑星科学部門、2.九州大学国際宇宙天気科学・教育センター、3.九州大学大学院理学府地球惑星科学専攻
1.Department of Earth and Planetary Sciences, Kyushu University, 2.International Center for Space
Weather Science and Education, 3.Gradational school of Earth and Planetary Sciences, Kyushu
University
For space environment monitoring, Kyushu University has developed a real time magnetic dataacquisition system (the MAGDAS project) around the world. The number of observational sites isincreasing every year with the collaboration of host countries. Now at this time, the MAGDAS
Project has installed 77 real time magnetometers –so it is the largest magnetometer array in theworld. The history of global observation at Kyushu Univ is over 30 years and number of developed
observational sites is over 140.
In this talk, we will introduce recent development of MGADAS project and stradegy for international
alliance of geomagnetic field network observation based on the project "Study of coupling processes
in solar-terrestrial system" that was approved by the Master Plan 2014 of Science Council of Japanand the Roadmap 2014 of MEXT.
Topics for open policy for MAGDAS data, development of Space weather index, and extension of
Equatorial network will be also discussed.
キーワード：国際協力、磁場ネットワーク観測、マスタープラン
Keywords: International aliance, geomagnetic field network, master plan

©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-09 -PEM09-10

日本地球惑星科学連合2016年大会

CHAMP衛星やSWARM衛星などの低高度衛星で観測される磁気リップル現象
Magnetic ripples as observed by low altitude satellites, CHAMP and SWARM*家森 俊彦1、中西 邦仁2、青山 忠司2、小田木 洋子1*Toshihiko Iyemori1, Kunihito Nakanishi2, Tadashi Aoyama2, Yoko Odagi1
1.京都大学大学院理学研究科付属地磁気世界資料解析センター、2.京都大学大学院理学研究科
1.Data Analysis Center for Geomagnetism and Space Magnetism, Graduate School of Science, Kyoto
University, 2.Graduate School of Science, Kyoto University
The low altitude satellites such as the CHAMP or the SWARM satellites have been observing the small
amplitude (typically 0.5 –5nT on the dayside) magnetic fluctuations with period of a couple of ten
seconds. They exist almost all the time and at any local time (LT) in middle and low latitudes.
They were named as “magnetic ripples” because the magnetic fluctuations like ripples exist
globally.
They have the following characteristics: (1) They are perpendicular to the geomagnetic main field.
(2) Their amplitude has the magnetic conjugacy. (3) The amplitude and the period along the orbit
have latitudinal dependence, and they depend also on the geographic longitude. (4) The amplitude islarger on the day side than on the night side. (5) The amplitude doesn’t have dependence on thesolar wind parameters nor the magnetic disturbance. (6) The amplitude has the following seasonal
and topographical characteristics. That is, the amplitude during the northern summer and northern
winter is larger than those during the equinoxes. In the northern summer, the amplitude over SouthAmerica, Eurasia, North Africa and Australia continents, and their magnetic conjugate regions islarger than those in the other regions. In the northern winter, the amplitude over the eastern
Pacific Ocean is larger.
We assume that they are generated through the E-region dynamo driven by the acoustic mode of thegravity waves propagated from lower atmosphere. We discuss the consistency of the above mentioned
characteristics and suggested mechanism of generation of the magnetic ripples with ground based
observations such as the GPS-TEC, micro-barometric observation, etc..
キーワード：磁気リップル、微細沿磁力線電流、重力音波、低高度磁場観測衛星
Keywords: magnetic ripples, small-scale field-aligned currents, acoustic gravity waves,
low-altitude magnetic satellite©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-10 -PEM09-11

日本地球惑星科学連合2016年大会

Observations of medium-scale traveling ionospheric disturbances using FORMOSAT-2 / ISUAL
630.0 nm airglow*Charles Lin1, P. K. Rajesh1, Jann-Yenq Liu2
1.Department of Earth Science, National Cheng Kung University, 2.Institute of Space Science,
National Central University, Chung-Li 320, Taiwan
We reports observation results of space based imaging of medium-scale travelling ionosphericdisturbances (MSTID) in 630.0 nm emission by Imager of Sprites and Upper Atmospheric Lightnings(ISUAL), onboard FORMOSAT-2 satellite. The limb integrated measurements, after removing background,reveal multiple bands of intensity perturbation when projected to a horizontal plane corresponding
to the altitude of peak emission, with distinct southwest to northeast orientation in the southernhemisphere. The ISUAL observations in the year 2007 are further used to investigate the MSTID
features as well as occurrence characteristics in the southern hemisphere, most of which are over
the ocean where no ground based observations are available. The preliminary statistics shows more
MSTID occurrence in solstices with peak in June-July months. Majority of the MSTID perturbations
have wavelength in the range 150-300 km, and are aligned at about 30°-50° from the east-west plane.
The orientation of the wave fronts indicate that Es-layer instability might be important in the
MSTID generation.
Keywords: MSTID, FORMOSAT-2/ISUAL, airglow©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-11 -PEM09-12

日本地球惑星科学連合2016年大会

国際共同観測およびモデルに基づく南北両半球結合過程の研究 (ICSOM)Interhemispheric Coupling Study by Observations and Modelling (ICSOM)*佐藤 薫1*Kaoru Sato1
1.東京大学

大学院理学系研究科

地球惑星科学専攻

1.Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo
Recent observational and modelling studies suggest that the Northern and Southern Hemispheres ofthe earth atmosphere are potentially coupled by the Lagrangian mean flow in the mesospheremodulated by waves interacting with the mean flow. However, observations of modulated wave and flow
fields which are needed for quantitative understanding of the interhemispheric coupling are notsufficient. Simultaneous observations of gravity waves at various locations are most importantbecause they are a main driver of the Lagrangian mean flow in the mesosphere.
With the start of full system observation by the PANSY radar in the Antarctic in March 2015, a
global mesosphere-stratosphere-troposphere (MST) radar network extending from the Arctic to the
Antarctic has been realized. The MST radars are able to observe wind vectors with fine temporal andvertical resolutions including vertical wind components in the troposphere, stratosphere andmesosphere, although an observational gap of the middle and upper stratosphere remains. Thus, thecharacteristics of small-scale or short-period wave motions including gravity waves and themomentum fluxes associated with these waves can be estimated with a good accuracy.
In addition, recent high-resolution general circulation models enable an explicit simulation ofgravity waves under ideal and/or climatological boundary conditions and allow us to examine themomentum budget in the MST region including gravity waves, although their resolution is currently
not sufficient to resolve the entire gravity wave spectrum. Real atmosphere simulations utilizing
such high-resolution models are still a challenge for the MST region. However, if such real
atmosphere simulations are successful, they will help quantitative interpretation of the dynamical
fields observed by the MST radar network, and the observations will provide invaluable validation
data for the model improvement.
Therefore we will examine the interhemispheric coupling of the earth atmosphere through a
combination of simultaneous observations by networking the MST radars over the world andhigh-resolution model simulations of the observed atmosphere. The first international campaign was
performed in 22 January-17 February 2016. Two minor stratospheric warmings occurred in the Arctic.
The second one was a minor warming by its definition but the temperature at the north poleincreased by about 70 K in two days at 10 hPa. Seven MST radars over the world and a lot ofcomplementary observations were performed by more than 30 participants in eight countries.
Preliminary results from this campaign will be reported.
キーワード：南北半球結合、中層大気、成層圏突然昇温、MSTレーダー、大気大循環、重力波
Keywords: interhemispheric coupling, middle atmospehre, sudden stratospheric warming,
mesosphere-stratosphere-troposphere radars, general circulation, gravity waves©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-12 -PEM09-13

日本地球惑星科学連合2016年大会

EISCAT_3D計画の現状と日本の貢献
Current Status of EISCAT_3D and Japan's Contribution*宮岡 宏1、野澤 悟徳2、小川 泰信1、中村 卓司1、大山 伸一郎2、藤井 良一2、Heinselman Craig3*Hiroshi Miyaoka1, Satonori Nozawa2, Yasunobu Ogawa1, Takuji Nakamura1, Shin-ichiro Oyama2, Ryoichi
Fujii2, Craig Heinselman3
1.大学共同利用機関情報・システム研究機構国立極地研究所、2.名古屋大学宇宙地球環境研究所、3.EISCAT科学協会
1.National Institute of Polar Research, 2.Institute for Space-Earth Environmental Research, Nagoya
University, 3.European Incoherent Scatter Scientific Association
The European Incoherent Scatter(EISCAT) Scientific Association with associate members from Sweden,
Norway, Finland, UK, China and Japan, including affiliated member organizations from South Korea,
France and EC, is planning for the construction of the next generation near-earth space and upper
atmosphere radar system in northern Feno-Scandinavia, called EISCAT_3D. The technical design work
is currently being almost finalized and the project has now entered the new phase of productionengineering. The Swedish Research Council, the Academy of Finland, the Research Council of Norway
and the European Commission have now granted funds for the development, construction and operationof EISCAT_3D, which covers approximately 70% of the total costs of establishing the first stage ofthe system. EISCAT_3D is the major upgrade of the existing EISCAT mainlamd radars, with amulti-static phased array system composed of one central active (transmit-receive) site and 4
receive-only sites to provide us 50-100 times higher temporal resolution than the present system.
The construction of EISCAT_3D is planned to implement by 4-staged approach, starting from the coresite with half transmitting power about 5MW at Skibotn (Norway) and 2 receiving sites at Bergfors(Sweden) and Karesuvanto (Finland) at the 1st stage. The Japanese EISCAT user community has been
pursuing the opportunity to contribute in-kind to the construction of EISCAT_3D. Our proposal is tosupply the power amplifiers for the radar as a joint venture with EISCAT in cooperation withJapanese industry. The EISCAT_3D program in Japan has been successfully granted as as one of 27
high-priority programs of Master Plan 2014 and 10 new Roadmap 2014 programs as a part of ’Study of
Coupling Processes in the Solar-Terrestrial System’ (PI: Prof. Tsuda, Kyoto Univ.). Supported bythis decision, National Institute of Polar Research has made a funding proposal to MEXT for
EISCAT_3D, collaborating with Institute for Space-Earth Environmental Research, Nagoya University.
In parallel to the funding proposal, we started a development for a high energy-efficient power
amplifier collaborating with the EISCAT headquarter and Japanese industry. In this paper, we will
overview the current status and outlook on Japan’s national contribution to the EISCAT_3D project.
Figure. Location of existing EISCAT radar and planned EISCAT_3D radar sites.
キーワード：非干渉散乱、レーダー、北極、ジオスペース
Keywords: incoherent scatter, radar, arctic, geospace©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-13 -PEM09-13©2016. Japan Geoscience Union. All Right Reserved.

日本地球惑星科学連合2016年大会- PEM09-13 -PEM09-14

日本地球惑星科学連合2016年大会

Significance of the D-region ion chemistry in the atmospheric forcing from above by
precipitating high-energy particles*Esa Turunen1
1.Sodankyla Geophysical Observatory, University of Oulu
Although the ionisation degree of middle atmosphere -lowere thermosphere region is low, it
surprisingly turns out that ion chemistry plays a significant role in causing variations inconcentrations of neutral chemically active minor constituents during events of excess ionisation,such as auroral particle precipitation. Here we first give an overview of the D-region ion
chemistry, pointing out the relevant processes, which can be both direct and indirect via first
generating chemically active minor constituents of the atmosphere, such as odd nitrogen and oddhydrogen, which in turn can affect for example atmospheric ozone via catalytic reactions either
directly in-situ, or after transport in atmosphere to lower altitudes and lower latitudes. We show
recent results using the detailed coupled neutral and ion chemistry model, the Sodankyla Ion
Chemistry model. We also show how the upcoming new incoherent scatter radar facility EISCAT_3D,
together with coordinated other currently planned measurements, will enhance the research
opportunity in studying the coupling between geospace environment and atmosphere of Earth duringhigh energy particle precipitation into the atmosphere.
Keywords: Ion chemistry, D region, aurora©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-14 -PEM09-15

日本地球惑星科学連合2016年大会

EISCAT、MF、流星レーダー、およびナトリウムライダーデータを用いた2016年2月における北極域下部熱圏・中間圏変動の研究
Variations of the polar lower thermosphere and mesosphere in February 2016 using EISCAT
radar, meteor radar, MF radar, and sodium LIDAR observations*野澤 悟徳1、小川 泰信2、津田 卓雄3、藤原 均4、堤 雅基2、ホール クリス5、ブハート ステファン6、斎藤徳人7、和田 智之7、川原 琢也8、高橋 透3、川端 哲也1、日比野 辰哉1、滝田 真太郎1、ブレッケ アスゲイル5*Satonori Nozawa1, Yasunobu Ogawa2, Takuo T. Tsuda3, Hitoshi Fujiwara4, Masaki Tsutsumi2, Chris Hall5, Stephan Buchert6, Norihito Saito7, Satoshi Wada7, Takuya Kawahara8, Toru Takahashi3, Tetsuya
Kawabata1, Tatsuya HIBINO1, Shintaro Takita1, Asgeir Brekke5
1.名古屋大学宇宙地球環境研究所、2.国立極地研究所、3.電気通信大学、4.成蹊大学、5.トロムソ大学、6.ス
ウェーデン宇宙物理研究所ウプサラ支部、7.理化学研究所、8.信州大学
1.Institute for Space-Earth Environment Research, Nagoya University, 2.NIPR, 3.The University ofElectro-Communications, 4.Seikei University, 5.UiT The Arctic University of Norway, 6.Swedish
Institute of Space Physics, 7.RIKEN, 8.Shinshu University
We made an EISCAT special program (SP) experiment, under collaborations of Japan, Sweden, andNorway, to study variations of a quasi-two day wave (Q2DW) and tidal waves in the polar lower
thermosphere using the EISCAT UHF radar at Tromsoe (69.6N, 19.2E) and the EISCAT Svalbard radar at
Longyearbyen (78.2N, 16.0E) for 45 hours. The SP started at 23 UT on February 10, 2016, just after
EISCAT CP2 (Common program 2) run made for 135 hrs, and ended at 20 UT on February 12, 2016. By
combining the EISCAT CP2 run and our SP run, we have, in total, made a data set of 7.5 day length.
Unfortunately, there was a data gap from about 01 UT to 07 UT on February 7 due to a problem ofdata recording at the Tromsoe site. Except for the gap, the operations went well without noseirouous problems at both the EISCAT radars. Sodium LIDAR observations of wind, temperature, andsodium density collocated at the Tromsoe site were also made during dark time intervals together
with meteor and MF radar contiunual observations. We have analyzed the data sets, and derived Q2DW
and 24h/12h tides. An SSW occurred in this time interval, so we focus on changes of the waves
around time interval of the SSW.
キーワード：下部熱圏、中間圏、大気潮汐波、準２日波、EISCATレーダー、ナトリウムライダー
Keywords: Lower thermosphere, Mesosphere, tidal waves, quasi-two data wave, EISCAT radar, sodium
LIDAR©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-15 -PEM09-P01

日本地球惑星科学連合2016年大会

MUレーダー実時間アダプティブクラッター抑圧システムの開発
Development of MU radar real-time processing system with adaptive clutter rejection*橋口 浩之1、万城 孝弘1、山本 衛1、佐藤 亨2、西村 耕司3、橋本 大志2*Hiroyuki Hashiguchi1, Takahiro Manjou1, Mamoru Yamamoto1, Toru Sato2, Koji Nishimura3, Taishi
Hashimoto2
1.京都大学生存圏研究所、2.京都大学情報学研究科、3.国立極地研究所
1.Research Institute for Sustainable Humanosphere, Kyoto University, 2.Graduate School ofInformatics, Kyoto University, 3.National Institute of Polar Research (NIPR)
大気レーダー観測において、しばしば強いクラッターエコー(山や建物からのエコー)が問題になることがある。そのクラッター抑圧法としてNC-DCMP (Norm Constrained-Directionally Constrained Minimum Power)法が提案され、MUレーダーによる実観測データに適用し、効果があることが実証されている[Nishimura et al.,JTech., 2012]。この処理は、これまではオフラインで実施されていた。そこで本研究では、NC-DCMP法によるクラッター抑圧処理をMUレーダーのオンライン処理システムとして実装することを目的とする。これにより、観測データの記録容量を数百分の１に削減でき、外部記憶装置などの制約の少ない標準観測を行うことが可能になる。NC-DCMP法では、所望信号方向を固定した上で、ウエイトベクトルのノルムをある値以下に制約して、信号電力を最小化するように制約条件付最適化問題を解く。
MUレーダーでは30年以上に渡って、毎月100時間程度の対流圏・成層圏標準観測モードによる観測を継続している。まず、この標準観測モードにNC-DCMP処理を実装した。このモードでの観測データは8秒に1回取得される。そのため、実時間でクラッター抑圧を行うためには全ての信号処理を8秒以内に行う必要があるが、処理方法の工夫により、NC-DCMP法の処理時間を平均1.0秒にまで高速化した。山や建物からのエコーは時間的に大きく変化しないため、インコヒーレント積分7回分(約1分間)の受信信号を用いて最適ウエイトベクトルを求めるようにしたところ、良好な結果を得た。2015年11月の標準観測からNC-DCMP処理を適用しているが、安定運用できている。完全ではないが、航空機からのエコーについても、抑圧する効果が得られている。
インドネシア共和国の西スマトラに建設が計画されている赤道MUレーダーは、八木アンテナ19本を1群とする
55群構成で、各群からの受信信号を独立に取得可能なシステムが提案されている。本研究の成果は、この赤道
MUレーダーにも適用可能である。
キーワード：大気レーダー、クラッター抑圧、ウエイトノルム拘束付DCMP法、MUレーダー
Keywords: Atmospheric radar, Clutter rejection, NC-DCMP method, MU radar©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P01 -PEM09-P02

日本地球惑星科学連合2016年大会

Variability of Rain Microstructure over Sumatra from Micro Rain Radar Observation*Marzuki Marzuki1, Indah Rahayu1, Hiroyuki Hashiguchi2, Toyoshi Shimomai3
1.Department of Physics, Andalas University, 2.Research Institute for Sustainable Humanosphere(RISH), Kyoto University, 3.Shimane University
The vertical profile of rain microstructure such as raindrop size distribution (DSD) is importantfor understanding rain formation processes and to improve the accuracy of radar-derived rainfall
estimates. The variability in the DSD substantially limits the accuracy of the DSD application. The
aim of the present study is to investigate the natural variability of vertical profile of DSDs as afunction of large-scale atmospheric conditions and storm characteristics using measurements fromthe Equatorial Atmospheric Radar (EAR) facility at Kototabang, west Sumatra, Indonesia. This study
is a follow-up of our previous work on the DSD variability over Sumatra [1,2]. The vertical profile
of DSD is obtained from a Micro Rain Radar (MRR) with a near continuous record of operation overfour consecutive years (2011–2014). The DSDs from the radar are compared with those from an optical
disdrometer. The data are partitioned according to diurnal, convective and stratiform precipitation
classifications, monsoonal regime, and MJO phase. Findings support previous Sumatra studies
suggesting a significant diurnal and DSD parameter signal associated with bothconvective–stratiform and MJO phase regime classification. Negligible monsoonal phase influence isdetermined for the DSD over the Kototabang location. The natural variability of vertical profile of
DSDs leads to variability of Z-R relationships in rain column.
[1] Marzuki, Hashiguchi, H., Yamamoto, M. K., Mori, S., and Yamanaka, M. D.: Regional variabilityof raindrop size distribution over Indonesia, Ann. Geophys., 31, 1941-1948,
doi:10.5194/angeo-31-1941-2013, 2013.
[2] Marzuki, Hiroyuki Hashiguchi, Toshiaki Kozu, Toyoshi Shimomai, Yoshiaki Shibagaki, Yukihiro
Takahashi, Precipitation microstructure in different Madden–Julian Oscillation phases over Sumatra,
Atmospheric Research, Volume 168, 1 February 2016, Pages 121-138.
Keywords: Raindrop size distribution, Micro Rain Radar, Sumatra©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P02 -PEM09-P03

日本地球惑星科学連合2016年大会

DIURNAL VARIABILITIES ANALYSIS OF METEOROLOGICAL PARAMETER OF CCAM-NWP OUTPUTS AND
OBSERVATION AT KOTOTABANG*Sofiati Iis Soeratman1, Lely Qodrita Avia1, Nurzaman Adikusumah1
1.Indonesian National Institute of Aeronautics and SpaceThe diurnal varibilities of some meteorological parameter (rainfall, temperature, relative
humidity, and pressure) study, needed a model that can predict the behavior of the weather in the
future by following the data history in the past. As a validation stage, outcomes such dynamic
model of spatial and temporal very necessary compared with surface observational data from
Automatic Weather Station (AWS) and u-v wind data from Equatorial Atmosphere Radar (EAR). The
purpose of this study is analyzing the diurnal varibilities of meteorological parameter of dynamic
model outputs Conformal Cubic Atmospheric Model-Numerical Weather Prediction (CCAM-NWP), and thesurface observational data. The data used is the hourly output CCAM-NWP models in (12-15) February,(12-15) June 2014, and (2-14) January 2015, and surface observational data in (2-4) January 2015 asvalidation. The method on analyzing the output CCAM-NWP from the input models Global Forecast
System (GFS-NOAA) with a resolution of the model 0.25o x 0.25o, and statistical analysis withmethod of T-test and F-test. Based on the results shown the diurnal variabilities and dinamic
process of meteorological parameter for the model output and surface observation. Furthermore, we
obtained a weak correlation between the temporal model output with surface observations fromstatistical analysis which mean that there are significant differences of the results found fromthe CCAM-NWP output and surface observations. Additionally, we compared spatial distribution ofhourly output CCAM-NWP with satellite observation data such as MTSAT.
Keywords: rainfall, temperature, relative humidity, pressure, CCAM-NWP, T-test, MTSAT.

©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P03 -PEM09-P04

日本地球惑星科学連合2016年大会

Solar-Terrestrial Interaction as Studied from Total Solar Eclipse of 9 March 2016
*Rhorom Priyatikanto1, Tiar Dani1, Emanuel Sungging Mumpuni1, Mamat Ruhimat1, Jiyo .1
1.Indonesian National Institute of Aeronautics and Space
Total Solar Eclipse of 9 March 2016 provides a great opportunity to study the interaction between
the Sun and Earth as a complex system. Several team of observers and scientists from National
Institute of Aeronautics and Space will be dispatched to some observing points along the track of
Lunar shadow and its proximity. The main missions are: (1) to study the physical nature of lower
part of Solar corona, (2) to understand the ionospheric disturbance caused by a sudden drop of
Solar radiation to the Earth, and (3) to measure the dynamics of local magnetic field that is
influenced by the ionospheric disturbance. Preliminary result of those observations/experiments
will be discussed in this paper.
Keywords: Solar Eclipse, Corona, Ionosphere, Geomagnet©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P04 -PEM09-P05

日本地球惑星科学連合2016年大会

RELATIONSHIP OF F LAYER HEIGHT RISE, ESF ONSET TIME, AND AMPLITUDE OF LARGE SCALE WAVE
STRUCTURE*Dyah Rahayu Martiningrum1, Mamoru Yamamoto2, Tatsuhiro Yokoyama3, Prayitno Abadi4, PornchaiSupnithi5, Minh Le Huy6
1.Graduate School of Informatics, Kyoto University, 2.Research Institute for Sustainable
Humanosphere, Kyoto University, 3.National Institute of Informatics and Communications Technology(NICT), Tokyo , 4.Solar-Terrestrial Environment Laboratory (STEL), Nagoya University, 5.Faculty ofEngineering King Mongkut's Institute of Technology, Ladkrabang, Thailand , 6.Institute ofGeophysics Vietnamese Academy of Science and Technology, Vietnam
Under favourable conditions ionospheric plasma at the bottomside of the F-region can become
unstable. Plasma irregularities in several scales produced by Rayleigh-Taylor Instability
mechanism. The recombination process at the E-region after sunset causing the bottom side F-region
electron density gradient become steep. At the same time the eastward electric field intensified
just before it reverses to the westward electric field causing the peak of the F region rise known
as evening prereversal enhancement. The relationship between onset time of field aligned
irregularities related to ESF observed by Equatorial Atmosphere Radar during 2010-2012 with F layerheight rise observed by ionosondes near geomagnetic equator, Chumphon (10.7 N; 99.4 E; 0.86 N) andBac Lieu (9.3 N; 105.7 E; 0.62 N) is discussed in correspondence with growth rate of Rayleigh
Taylor instability development. The field aligned irregularities onset time associated withequatorial spread F observed into two different cases, first case where the EPB/ESF onset time
concurrent with the peak of virtual height of F region - (h’F) time. Second case where the EPB/ESF
onset time happened with delay of more than 30 minutes, with reference to the peak of virtual
height of F region - (h’F) time. The possibility that the amplitude of Large Scale Wave Structure
obtained from GRBR data effects the height of plasma instability development also discussed.
Keywords: F layer height rise, Large Scale Wave Structure, onset time of Equatorial Spread F©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P05 -PEM09-P06

日本地球惑星科学連合2016年大会

EIA structure and its relation to plasma bubble occurrence along longitude 100° E in 2012
*Kornyanat Watthanasangmechai1, Mamoru Yamamoto2, Tatsuhiro Yokoyama1, Michi Nishioka1, Mamoru Ishii
11.National Institute of Information and Communications Technology, 2.RISH, Kyoto Univ.
To reveal a relationship between EIA structure and plasma bubble occurrence along longitude 100° E
in 2012, the ground-based observations i.e., GNU Radio Beacon Receivers (GRBR), GPS, ionosonde, andEquatorial Atmospheric Radar (EAR), are employed. GRBR is used to capture the precise structure of
EIA. The Rate Of TEC change Index (ROTI) of GPS is used to monitor the plasma bubble occurrence.
Temporal variation of the bottom side of the F layer is measured by the ionosonde. The EAR is for
detecting Field Aligned Irregularities (FAI). In this paper, we will answer the following
questions:(1) What does the EIA structure look like on the plasma bubble on and off day?
(2) Is it necessary that plasma bubble will occur only when EIA is symmetric?
(3) How does the plasma bubble structure look like on the GRBR TEC?
Keywords: EIA, Plasma bubble©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P06 -PEM09-P07

日本地球惑星科学連合2016年大会

TBExおよびFORMOSAT-7/COSMIC-3衛星を用いた赤道電離圏研究用の新ディジタルビーコン受信機
New digital beacon receiver for the study of equatorial ionosphere with satellites TBEx
and FORMOSAT-7/COSMIC-2*山本 衛1、岩田 桂一1、松永 真由美2、Tsunoda Roland3、Doe Richard3、Hsiao Tung-Yuan4*Mamoru Yamamoto1, Keiichi Iwata1, Mayumi Matsunaga2, Roland Tsunoda3, Richard Doe3, Tung-Yuan Hsiao4
1.京都大学生存圏研究所、2.愛媛大学理工学研究科、3.SRI International、4.Hsing Wu University
1.Research Institute for Sustainable Humanosphere, Kyoto University, 2.Graduate School of Scienceand Engineering, Ehime University, 3.SRI International, 4.Hsing Wu University
We have successfully conducted observations of total-electron content (TEC) of the ionosphere using
a satellite-to-ground beacon experiment. A unique dual-band (150/400MHz) digital receiver GRBR (GNURadio Beacon Receiver) was developed for this purpose, which is based on the recent digital-signal
processing technologies. The GRBR network was deployed into the southeast Asian and Pacificregions. By using beacon signals from the low-inclination satellite C/NOFS, we studied longitudinal“large-scale wave structures (LSWS)” in detail as a possible source of equatorial Spread-F (ESF)
events. Now there are 2 new beacon-satellite plans. One is TBEx (Tandem Beacon Explorer), a projectby SRI International, to fly a constellation of two 3U cubesats with triband beacon transmitters.
Another one is a constellation of FORMOSAT-7/COSMIC-2 satellites, also with triband (or quad-band)
beacon transmitters. All of these satellites will be placed into low-inclination orbits by the samelaunch vehicle in late 2016. This launch will provide great opportunities to enhance studies of the
low-latitude ionosphere. Kyoto University, Ehime University and Hsing Wu University are now
developing the new GRBR system that is expected to be used for the TBEx and FORMOSAT-7/COSMIC-2
beacon experiments. In the presentation we will show development of the new beacon receiver
together with plan of observations.
キーワード：衛星―地上ビーコン観測、電離圏全電子数、COSMIC-2、cubesat、赤道電離圏
Keywords: Satellite-ground beacon experiment, Ionospheric TEC, COSMIC-2, cubesat, equatorial
ionosphere©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P07 -PEM09-P08

日本地球惑星科学連合2016年大会

太陽地球結合系研究のためのIUGONETデータ解析システム
IUGONET data analysis system for a study of coupling processes in the solar-terrestrial
system
*新堀 淳樹1、田中 良昌2、梅村 宜生3、小山 幸伸4、阿部 修司6、能勢 正仁7、上野 悟5*Atsuki Shinbori1, Yoshimasa Tanaka2, Norio Umemura3, Yukinobu Koyama4, Shuji Abe6, Masahito Nose7,
Satoru UeNo5
1.京都大学生存圏研究所、2.国立極地研究所、3.名古屋大学宇宙地球環境研究所、4.新領域融合セン
ター、5.京都大学大学院理学研究科天文台、6.九州大学 国際宇宙天気科学・教育センター、7.京都大学大学院
理学研究科地磁気センター
1.Research Institute for Sustainable Humanosphere (RISH), Kyoto University, 2.National Institute ofPolar Research, 3.Institute for Space-Earth Environment research (ISEE), Nagoya University ,4.Transdisciplinary Research Integration Center, 5.Hida Observatory, Kyoto University, 6.
International Center for Space Weather Science and Education (ICSWSE), Kyushu University, 7.WDC for
Geomagnetism, Kyoto University
Various kinds of disturbance phenomenon and long-term variation in the upper atmosphere above 100
km are caused by energy input from solar radiation, solar wind, momenta and energies from the lower
atmosphere via atmospheric waves, and chemical reaction. Such a disturbance phenomenon andlong-term variation observed by various kinds of ground-based and satellite instruments are theresult of such complicated processes. Therefore, in order to understand the mechanisms of these
phenomena detected in this region, researchers need to conduct comprehensive analyses with various
kinds of long-term observation data that have been continued by means of a global network ofradars, magnetometers, optical sensors, helioscopes, etc. The IUGONET (Inter-university Upper
atmosphere Global Observation NETwork) project initiated in 2009 is proposed to establish across-reference system for various kinds of ground-based observation data obtained from different
techniques. The IUGONET participants consist of five universities/institutes: the National
Institute of Polar Research (NIPR), Tohoku University, Nagoya University, Kyoto University, andKyushu University. We have developed a metadata database (MDDB) and IUGONET data analysis software(UDAS) of ground-based observation data managed by these IUGONET universities/institutes with aninternational collaboration in order to promote a comprehensive study on coupling processes in the
Sun-Earth system. MDDB provides researchers in a wide range of disciplines with a seamless data
environment to link observation databases spread across the IUGONET universities/institutes.
Researchers can find basic information of observation data (for example, observation period, data
format, data use policy, instrument, observed region, observation site etc.) from the metadata foreach observation data they are interested in. Recently, the metadata for several satellite
observation data (for example, Akebono, GPS) have been registered to MDDB, and researcher caneasily find the satellite database. UDAS will also be of great help in conducting integrated
analyses and visualization of various kinds of solar-terrestrial observation data to investigate
the long-term variation in the upper atmosphere throughout the Sun-Earth system. UDAS deals with 29
kinds of ground-based observation data provided by the IUGONET universities/institutes. Moreover,the executable file of SPEDAS/UDAS working on Interactive Data Language (IDL)-VM without IDL
license has been released on the SPEDAS website. Owing to the executable file, anybody can use UDAS
and conduct a comprehensive analysis of various kinds of solar and Earth’s atmospheric observation
data. Moreover, in the IUGONET project, in order to enhance an international use of these IUGONET
products, we held a mini-training workshop of how to use the IUGONET MDDB and UDAS at several
developing countries (India, Indonesia, Nigeria, Peru etc). Now, the IUGONET products became an©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P08 -PEM09-P08

日本地球惑星科学連合2016年大会

essential tool to study a mechanism of the solar-terrestrial environmental change. In this talk, we
introduce a brief overview of the IUGONET project, and an application of the IUGONET products totypical examples of upper atmospheric researches.
キーワード：大学間連携プロジェクト(IUGONET)、超高層大気、メタデータデータベース、解析ソフト、長期変動、地上観測Keywords: Inter-university Upper atmosphere Global Observation NETwork, Upper atmosphere, Metadata
database, IUGONET data analysis software (UDAS), Long-term variation, Ground-based
observation©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P08 -PEM09-P09

日本地球惑星科学連合2016年大会

Ionospheric weather in the dayside polar cap region*Hitoshi Fujiwara1, Satonori Nozawa2, Yasunobu Ogawa3, Ryuho Kataoka3, Yasunobu Miyoshi4, Hidekatsu
Jin5, Hiroyuki Shinagawa5, Huixin Liu4
1.Faculty of Science and Technology, Seikei University, 2.Institute for Space-Earth Environment
Research, Nagoya University, 3.National Institute of Polar Research, 4.Department of Earth andPlanetary Sciences, Faculty of Sciences, Kyushu University, 5.National Institute of Information andCommunications Technology
Using European incoherent scatter radar (EISCAT) and EISCAT Svalbard radar (ESR),
we have made simultaneous obserbations of the dayside polar cap ionosphere atLongyearbyen and Tromso. Five year observation data show significant disturbancesin the polar cap region northward the ESR site even during geomagnetically quiet
periods. This suggests that the energy input from the magnetosphere would playa fundamental role for dynamics and energetics in the region all the time. In
addition, some researchers suggest effects from the lower atmosphere on thethermospheric variations in the polar region. In order to understand variationsof the polar ionosphere/thermosphere from hour to hour, we should understandenergy flows from the above (magnetosphere) and below (lower atmosphere).
Numerical simulations with a GCM are also essential to do so. In particular,
GCM simulations would reveal physical and chemical processes/mechanisms
to produce the thermoshperic variations while the thermospheric observations
are very few in the dayside.
In the present study, we overview the EISCAT and ESR observations during 2011-2016.
The recent progress of our understandings from comprehensive observations andGCM simulations are also shown.
Keywords: ionosphere, thermosphere, EISCAT, GCM, simulation©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P09 -PEM09-P10

日本地球惑星科学連合2016年大会

Using Vondrak smoothing method to improve the prediction of Sunspot Maximum*ZQ Yin1, YB Han1
1.NAO. CAS. CHINA
About 11-year cycle of solar activity is the most significant quasi-periodic component, whichlargely represents the strength of solar activity and is the basis for dividing solar cycle. Many
studies have proven that solar activity can affect the developing process of many phenomena on the
Earth, such as climate, geophysical and marine changes etc. In order to meet the demands ofheliophysics and solar activity variation characteristics studies, especially, for the demand of
Solar Terrestrial Relations studies and space science development, studies of solar activity
characteristics and prediction are getting more attention. Some authors summerized a variety ofmethods for the maximum predictions of 22nd, 23rd, 24th solar cycles, the incomplete statistics are
63, 54 and 75 cases respectively, results of the methods, which the difference between forecastingand observed values within the range of ±15%, are 27.0%, 25.9% and 24.3% respectively. Using the 13
points smoothed value of monthly sunspot numbers, we studied correlation between sunspot number
rising rate of the first 24 months of the solar cycle and the coming cycle maximum, publishedforecasting result that the maximum value was 139.2 ±18.8 for 23rd solar cycle (Han et al., 2000),
and the observed value is 120.8, the error is about 15.2%. The present paper introduces our
improved forecasting methods. Vondrak smoothing method is used to deal with the monthly sunspot
numbers. It is studied that the relationship between the rise rate of earlier months of sunspot
numbers of this smoothed sequence and the coming maximum value in each solar cycles. The results
show that the first 22, 23, 24 months rise rate of sunspot numbers are highly related with thecoming maximum values, and simulated prediction of maximum for 22~24 cycles show that using the
22-month rise rate of three solar cycles, the maximum forecasting error is about 13.2%, using
23-month rise rate, the maximum error is about 11.2%, while using 24-month rise rate, the maximum
error is only about 9.3%. The new method can make the forecasting time in advance at least half ayear than the common method using 13 points monthly smoothed value, which the difference between
prediction and observed values within the range of ±15%. The results also show that the maximum
error is about 20% if we use 18-month rise rate, and it can make the forecasting time in advance atleast one year than the common method using 13 points monthly smoothed value.
Keywords: Sunspot Maximum, Prediction©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P10 -PEM09-P11

日本地球惑星科学連合2016年大会

D- and E-region ISR spectra measured with the EISCAT radars
D- and E-region ISR spectra measured with EISCAT radars*小川 泰信1、野澤 悟徳2、Häggström Ingemar3*Yasunobu Ogawa1, Satonori Nozawa2, Ingemar Häggström 3
1.国立極地研究所、2.名古屋大学宇宙地球環境研究所、3.EISCAT本部
1.National Institute of Polar Research, 2.Institute for Space-Earth Environmental Research, Nagoya
University , 3.EISCAT Headquarters
The energy from the solar wind is mainly transported to the polar upper atmosphere and causes
various phenomena such as auroras characterized by their rapid variability in time and space.
Incoherent scatter radar (ISR) located in high latitude is one of the most powerful tools toinvestigate generation mechanisms of such phenomena and their effects on the atmosphere. The ISR
basically gives information of plasma parameters between the bottom-side and topside ionospheres.
However, the ISR has several unavoidable limitations to derive ionospheric parameters in the E- andD-region ionospheres, due to limited information of the ISR spectra.
We have investigated ISR spectra in the D- and E-region using the latest techniques of the EISCAT
UHF and VHF radars located in Tromsø. Previous studies indicate that the EISCAT UHF and VHF radars
have limitations of plasma parameter derivation below 90 and 100 km altitudes, respectively. We
show lower limits of reliable plasma parameter derivation using the latest pulse coding techniquesof the EISCAT radars. Based on the knowledge and experience of the current EISCAT radarobservations, we will discuss possibility and limitation of future E- and D-region observations of
the EISCAT_3D radar.
キーワード：ionosphere、Incoherent scatter radar、plasma
Keywords: ionosphere, Incoherent scatter radar, plasma©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P11 -PEM09-P12

日本地球惑星科学連合2016年大会

トロムソOMTIを用いた極域超高層大気の国内・国際共同研究
National/International joint studies with the Tromsø OMTI for studying the polar upper
atmosphere*大山 伸一郎1、塩川 和夫1、野澤 悟徳1、大塚 雄一1、三好 由純1、Turunen Esa2、Aikio Anita3、Cai Lei3
*Shin-ichiro Oyama1, Kazuo Shiokawa1, Satonori Nozawa1, Yuichi Otsuka1, Yoshizumi Miyoshi1, Esa
Turunen2, Anita Aikio3, Lei Cai3
1.名古屋大学宇宙地球環境研究所、2.オウル大学ソダンキラ地球物理学観測所、3.オウル大学
1.Institute for Space-Earth Environmental Research, Nagoya University, 2.Sodankyla GeophysicalObservatory, University of Oulu, 3.University of Oulu
Institute for Space-Earth Environmental Research (ISEE) has been operating various kinds of optical
instruments for more than 15 years at the Tromsø European Incoherent Scatter (EISCAT) radar site in
Norway (Geographic: 69.6N, 19.2E, Geomagnetic: 66.7N, 102.2E, L=6.4), which is one of thestate-of-art observatories at high latitudes. In January 2009, we began operation of a Fabry-Perot
interferometer (FPI) and an all-sky type cooled CCD camera (ASC) at dark nights of the wintermonths (from middle of September to early April in most years). The FPI (#01 of the Optical
Mesosphere Thermosphere Imagers (OMTIs)) measures airglow and aurora by rotationally changing
optical wavelengths of 557.7 and 630.0 nm for most of the nights in order to derive thethermospheric wind and temperature. Four cardinal points with zenith angle of 45 or 15 and thegeographic vertical (i.e. five directions) are measured sequentially. The combination of data fromthe four cardinal positions provides the horizontal components of the neutral wind velocity. The
all-sky camera (camera #12 of OMTIs) includes a filter wheel used to select one of the six opticalfilters (channel 1: 557.7 nm, channel 2: 630.0 nm, channel 3: OH band (720 ∼1000 nm), channel 4:589.3 nm, channel 5: 572.5 nm, and channel 6: 732.0 nm). While the exposure time for FPI and ASC
measurements is tuned as good for individual scientific objectives, in the case of FPI typicalvalues are 1 minute or 15 seconds for airglow and auroral measurements, respectively, and in thecase of ASC those are about 30 and 10 seconds for the individual targets, respectively. However,shorter exposure times have been applied for measuring fine structures of aurora. Other optical
instruments such as photometer, digital camera, and all-sky camera (486.1 nm) are collocated with
the OMTI FPI and ASC. Data from these instruments have been provided to national and international
researching activities. For example, the FPI was operated together with the EISCAT radars as a key
diagnostic instrument for providing thermospheric parameters during periods of geomagnetic
disturbances. Integrated studies of the FPI-measured wind and the EISCAT-measured ionosphericparameters (including full vector of the electric field) improve our understanding of the energy
dissipation and momentum transfer processes and of polar ionospheric/thermospheric responses to thesolar-wind change. Effects of energetic electron precipitation (EEP) on the atmosphere are also
analyzed using data from our optical instruments and EISCAT radars. This topic is proceeded undercollaboration with Chemical Aeronomy in the Mesosphere and Ozone in the Stratosphere (CHAMOS)
group. Sodankylä Ion Chemistry (SIC) model, which is used in the group, is a powerful tool for
estimating atmospheric responses to EEP, in particular variations in the atmospheric minor
components such as NOx, HOx, and O3. Ionospheric and atmospheric variations associated with EEP will
be one of the important scientific objectives in the ERG project. This presentation will make abrief introduction of a few results from the national/international join studies.
キーワード：オーロラ、大気光、光学装置、電離圏、熱圏、高緯度©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P12 -PEM09-P12

日本地球惑星科学連合2016年大会

Keywords: Aurora, Airglow, Optical instrument, Ionosphere, Thermosphere, High latitude©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P12 -PEM09-P13

日本地球惑星科学連合2016年大会

脈動オーロラが起こすナトリウム密度変動の研究: 高速ナトリウムライダー観測
Study on pulsating aurora-induced sodium density variation: high-speed sodium lidar
observation*高橋 透1、津田 卓雄2、細川 敬祐2、野澤 悟徳3、小川 泰信4、川原 琢也5、斎藤 徳人6、和田 智之6、川端
哲也3、Hall Chris7*Toru Takahashi1, Takuo T. Tsuda2, Keisuke Hosokawa2, Satonori Nozawa3, Yasunobu Ogawa4, Takuya
Kawahara5, Norihito Saito6, Satoshi Wada6, Tetsuya Kawabata3, Chris Hall7
1.電気通信大学宇宙・電磁環境研究センター、2.電気通信大学大学院情報理工学研究科、3.名古屋大学宇宙地球環境研究所、4.国立極地研究所、5.信州大学工学部、6.理化学研究所、7.トロムソ大学
1.Center for Space Science and Radio Engineering, The University of Electro-communications,
2.Department of Communication Engineering and Informatics, University of Electro-Communications,
3.Institute for Space-Earth Environment Research, 4.National Institute of Polar Research, 5.Facultyof Engineering, Shinshu University, 6.RIKEN, 7.The Arctic University of Norway
トロムソナトリウムライダーは2010年10月に観測を開始し，2016年2月現在までの冬季に計6シーズンの観測を行っている。これまで、EISCAT観測所に設置された観測機器との同時観測データを用いて、大気重力波の上方伝搬、イオン温度と中性大気温度の比較、スポラディックナトリウム層の生成機構など数分から数時間の時間スケールの現象を取り扱ってきた。
近年、高エネルギー電子を振り込ませる脈動オーロラが注目されつつある。脈動オーロラを起こす高エネル
ギー電子は高度100 km以下まで侵入し、衝突を介して中性大気にエネルギーを受け渡す。このエネルギーの授受に伴う中性大気の応答過程は未だに明らかになっていない。これは、明滅周期が10秒前後である脈動オーロ
ラに対して、十分な時間分解能で中性大気を計測するような観測が行われていないことに大きな問題があるためである．
本研究では、高出力・高感度のトロムソナトリウムライダーのデータ取得系及び、レーザー制御系に改良を加え、現システムの時間分解能を１桁以上向上させることに挑戦した。国内で開発した改良データ記録システムを2016年１月にトロムソのライダーシステムに導入し、試験的な観測をすでに開始，現在では秒/サブ秒
オーダーでのナトリウム密度計測に成功している。本発表では、2015年1月〜3月の試験的観測により得られたナトリウム密度の高時間分解能データの紹介を行う予定である。
キーワード：ナトリウムライダー、脈動オーロラ
Keywords: sodium lidar, pulsating aurora©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P13 -PEM09-P14

日本地球惑星科学連合2016年大会

南極昭和基地大型大気レーダーで得られた中間圏エコーと下部電離圏における電子密度モデルとの比較研究Comparison study between coherent radar echo and empirically-modeled electron density inthe mesosphere based on the PANSY radar*西山 尚典1,2、佐藤 薫3、中村 卓司1,2、堤 雅基1,2、佐藤 亨4、西村 耕司1,2、田中 良昌1,2、冨川 喜弘1,2、高麗 正史3*Takanori Nishiyama1,2, Kaoru Sato3, Takuji Nakamura1,2, Masaki Tsutsumi1,2, Toru Sato4, Koji
Nishimura1,2, Yoshimasa Tanaka1,2, Yoshihiro Tomikawa1,2, Masashi Kohma3
1.国立極地研究所、2.総合研究大学院大学、3.東京大学、4.京都大学
1.National Institute of Polar Research, 2.SOKENDAI (The Graduate University for Advanced Studies),
3.The University of Tokyo, 4.Kyoto University
Polar Mesosphere Winter Echo (PMWE) is known as back scatter echo from 55 to 85 km in themesosphere, and it has been observed by MST and IS radar in polar region during non-summer period.
Since density of free electrons as scatterer is low in the dark mesosphere during winter, it issuggested that PMWE requires strong ionization of neutral atmosphere associated with Energetic
Particles Precipitations (EPPs) during Solar Proton Events [Kirkwood et al., 2002] or during
geomagnetically disturbed periods [Nishiyama et al., 2015]. However, studies on relationshipbetween occurrence of PMWE and background electron density has been limited yet [Lübken et al.,2006], partly because the PMWE occurrence rate is known to be quite low (2.9%) [Zeller et al.,2006].
The PANSY (Program of the Antarctic Syowa MST/IS) radar, which is the largest MST radar in
Antarctica, observed many PMWE events since it has started mesosphere observations in June 2012. We
established an application method of the PANSY radar as riometer, which makes it possible toestimate Cosmic Noise Absorptions (CNA) as proxy of relative variations on background electron
density. In addition, electron density profiles from 60 to 150 km altitude are calculated by
Ionospheric Model for the Auroral Zone (IMAZ) [McKinnell and Friedrich, 2007] and CNA estimated by
the PANSY radar.
In this presentation, we would like to focus on strong PMWE during two big geomagnetic storm
events, St. Patrick’s Day and the Summer Solstice 2015 Event, in oreder to compare observed PMWE
characteristics to model background electron density. On March 19 and 22, recovery phase of St.
Patrick’s Day Storm, sudden PMWE intensification was detected near 60 km by the PANSY radar. At thesame time, strong Cosmic Noise Absorptions (CNA) of ~ 0.8 dB and 1.0 dB were measured,
respectively. However, calculated elctron density profiles did not necessarily demonstrate highelecetron density at the altitude where the PMWE intensifications were observed. On June 22, theSummer Solstice 2015 Event, strong nighttime PMWE near 80 km was detected around 16 UT, which isequal to 19 LT at Syowa station. Since PMWE observations are primarily confined to daytime becauseof relatively abundant free electrons in the illuminated mesosphere, this strong and long-lived
nighttime PMWE implies that EPPs related to the storm caused the sporadic ionization sufficient for
PMWE even in dark mesosphere. The modeled electron density profile agreed with the occurrence of
the PMWE, showing density enehancement of 109 - 1010 cm-3 from 60 to 80 km altitude. The difference
between the above two events is thought to be caused by overestimations of CNA in St. Patrick’s Day
Storm, which leads to underestimation of modeled electron density. We are going to validate CNA
estimated by the PANSY radar and discuss about discrepansy between modeled elecron density and PMWE
in detail.

©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P14 -PEM09-P14

日本地球惑星科学連合2016年大会

キーワード：大型大気レーダー、中間圏、冬季極域中間圏エコー、電離圏D領域
Keywords: MST radar, Mesosphere, Polar Mesosphere Winter Echo, Ionopheric D-region©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P14 -PEM09-P15

日本地球惑星科学連合2016年大会

南極昭和基地SENSU SuperDARNレーダーの第Ⅸ期南極研究観測計画(2016-2023)
Antarctic Syowa station SENSU SuperDARN radars in the 9th phase of JARE Atarctic project(2016-2023)*行松 彰1,2*Akira Sessai Yukimatu1,2
1.国立極地研究所、2.総合研究大学院大学
1.National Institute of Polar Research, 2.Dept. Polar Sci., SOKENDAI (The Graduate University for
Advanced Studies)
Syowa SENSU SuperDARN HF radars are important components of SuperDARN, the international HF radars
network since 1995 and have significantly contributed to understanding not only
magnetosphere-ionosphere coupling system but also MLT region dynamics. As SuperDARN radars wereoriginally designed to reveal global polar ionospheric plasma convection patterns in bothhemispheres in real time, its spatial resolution has been relatively low. As the number of newscientific targets like comparison with mid and small scale aurora phenomena, meso scale transientphenomena, elementary generation and decay process of field aligned irregularities, PMSEs and fineheight profile of neutral wind has been increasing, higher spatial and temporal resolution
observations have been essentially desired and of great importance. Imaging radar technique has
been tried to be applied and developed to overcome these issues. We show the current status of the
SENSU imaging radar system, and will discuss particularly on the scientific targets including
coming JARE (Japanese Antarctic Research Expedition) project phase IX (2016-2023) and the future
perspectives which can be revealed by this new technique using SuperDARN. In the phase IX JARE
project. Our research group has proposed a research program to JARE project focused especially on
possible grand minimum influences on geospace environment and inner magnetospheric dynamics and thedetail plans including collaboration with other satellite and ground-based observation and its
contribution to the project "Study of coupling processes in solar-terrestrial system" as well as
the international VarSITI program will be discussed.
キーワード：SuperDARN、南極昭和基地、第Ⅸ期南極観測計画、グランドミニマム、内部磁気圏、VarSITI
Keywords: SuperDARN, Antarctic Syowa Station, Japanese Antarctic Research Expedition project phase
9, Grand minimum, inner magnetosphere, VarSITI©2016. Japan Geoscience Union. All Right Reserved.

- PEM09-P15 -