Commission G: Ionospheric Radio and Propagation (November 2013 – October 2016)
Edited by Mamoru Yamamoto

URSI Commission G takes care of radio propagation in the ionosphere and the study of the ionosphere
and/or upper atmosphere. In this national report, we would like to summarize the research activities byshowing major measurement instruments, observation network, related model/database projects, and futureplans that are closely related to the Commission G. For results of the studies, please refer to papers that arelisted below.

G.1 Major Instruments
G1.1 PANSYPANSY (Program of the Antarctic Syowa MST/IS Radar) is a project which was started in 2000 tocomprehensively study the polar atmosphere with a large aperture atmospheric radar as the main instrument
combined with complementary observation techniques and also with numerical modeling and theoreticalworks. (PANSY project web page: http://pansy.eps.s.u-tokyo.ac.jp/en/)
The radar started research observation in 2012 with 1/4 of the full array system, and has collected almost
continuous observational data in the troposphere, lower stratosphere and mesosphere for about three years.
Although the full system operation has been postponed due to limited transportation in 2011/12 and 2012/13
seasons caused by a very thick sea-ice condition, full system observations have been successfully started inearly 2015 with 520 kW transmitting power and 1045 array antennas.
1-year continuous full system observation of the PANSY radar started late September 2015. It enables
us to capture various temporal- and spatial-scale phenomena in the Antarctic troposphere, stratosphere,
mesosphere, and thermosphere/ionosphere with high temporal and vertical resolution throughout the year
and to contribute to improving global climate models for better understanding of future climate change.
In addition, the first international campaign based on a combination of GCM (General Circulation
Model) simulations and simultaneous observations by several MST/IS radars over the world including
PANSY and some complementary instruments such as MF (Medium Frequency) and meteor radars, lidars,
imagers, and so on was successfully conducted from January 22 to February 17, 2016. This campaign wasnamed the Interhemispheric Coupling Study by Observations and Modeling (ICSOM: see details at
http://pansy.eps.s.u-tokyo.ac.jp/icsom/), and approved as a project for ROSMIC (Role Of the Sun and the
Middle atmosphere/thermosphere/ionosphere In Climate) of SCOSTEP (Scientific Committee on SolarTerrestrial Physics) under ICSU (International Council for Science). It is expected that these international
collaborations including the PANSY radar will promote a more accurate understanding of the Antarctic
atmosphere and interhemispheric coupling processes.

G1.2 EISCAT radar
NIPR (National Institute of Polar Research) and Institute of Space-Earth Environmental Research,
Nagoya University have joined the EISCAT (European Incoherent Scatter) Scientific Association since 1996
and conducted observations with three incoherent scatter radar systems, at 224 MHz, 931 MHz in Northern
Scandinavia and one at 500 MHz on Svalbard. They kept high research activity in this period. Examples ofresearch results are as follows. (EISCAT database in NIPR: http://pc115.seg20.nipr.ac.jp/www/eiscatdata/)
Ogawa et al (2014) studied data from the EISCAT radar above Tromsø for over 33 years, and estimatedthe first significant trends of ion temperature at altitudes between 200 and 450 km. The estimated trends
indicate a cooling of 10–15 K/decade near the F region peak (220–380 km altitude), whereas above 400 km
the trend is nearly zero or even warming. Miyoshi et al (2015) showed that pulsating auroras show quasiperiodic intensity modulations caused by the precipitation of energetic electrons of the order of tens of keV.
It is expected theoretically that not only these electrons but also sub-relativistic/relativistic electrons
precipitate simultaneously into the ionosphere owing to whistler-mode wave-particle interactions. Iyeda etal (2015) studied the solar zenith angle (SZA) dependence of the conductance, and obtained a simple

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theoretical form for the Hall-to-Pedersen conductance ratio, using the peak plasma production height basedon observations with the EISCAT radar at Tromsø. Taguchi et al (2015) reported three-dimensional imagingof the plasma parameters of a moving cusp aurora from the all-sky imager at Longyearbyen, Svalbard. Also,
Nozawa et al (2014) reported that a new solid-state sodium lidar installed at Ramfjordmoen, Tromsø (69.6°N,
19.2°E), started observations of neutral temperature together with sodium density in the mesosphere-lower
thermosphere (MLT) region on 1 October 2010.

G1.3 SuperDARN Hokkaido East / West Radars
SuperDARN (Super Dual Auroral Radar Network) is an international collaboration project by elevencountries in the world. Most SuperDARN radars have observed the polar regions higher than 60 geomagnetic
latitude for more than a decade. The mid-latitude SuperDARN radars began operation recently (since 2005),
and new discoveries have been made using newly constructed SuperDARN radars by several countries in
the world such as Japan, USA and UK. The Hokkaido East / West radars were constructed by Nagoya
University in 2006 / 2014, and are located in the lowest latitude of the recently constructed radars. Detailed
information of this radar is found from: http://cicr.isee.nagoya-u.ac.jp/hokkaido/index.html
The radars are used for variety of studies of the magnetosphere and the ionosphere. In the ionosphericregion, the study of the traveling ionospheric disturbance (TID) is the important topic. During the period of
2014-2016, medium-scale TIDs (MSTIDs) were intensively studied. For example, Koustov et al. (2014)
investigated 117 of periodic E region echoes that propagate, for 2008-2012. The wave structures, which are
actually MSTIDs, are shown to occur at nighttime, preferentially during summer, although significant
number for events was found for winter. They interpreted the onset of these MSTIDs in terms of gravity
waves. Oinats et al (2016) further conducted statistical study of MSTIDs using the Hokkaido East (2007 to2014) and Ekaterinburg (2013 to 2014) high-frequency (HF) radar data, and compared their propagation
directions with that of the ambient neutral wind.

G1.4 MU radar
The MU radar is the 46.5-MHz atmospheric radar located in Shigaraki, Shiga, Japan. The radar canmeasure atmospheric winds from near the surface to about 20km, and is also useful to measure coherent andincoherent scatters from the ionosphere. Multi-beam capability with the active-phased array antenna is themost power feature of the system, and the various interesting observations were conducted so far. (MU radarand EAR web: http://www.rish.kyoto-u.ac.jp/mu+ear/english/index.html)
IEEE, an association dedicated to advancing innovation and technological excellence for the benefit ofhumanity, is the world’s largest technical professional society. IEEE established the Milestones Program in1983 to recognize the achievements of the Century of Giants who formed the profession and technologies
represented by IEEE. Each milestone recognizes a significant technical achievement that occurred at least
25 years ago in an area of technology and having at least regional impact. In December 2014, IEEE decided
to award Milestone to the MU (Middle and Upper atmosphere) radar as the first large-scale MST(Mesosphere, Stratosphere, and Troposphere) radar with a two-dimensional active phased array antenna
system. The MU radar was established in 1984 by Kyoto University with collaboration of Mitsubishi Electric
Corporation, and enabled continuous and flexible observation of the atmosphere, and has contributed to theprogress of atmospheric science and radar engineering. Its dedication ceremony was successfully held on
May 13, 2015 at Shirankaikan, Kyoto University.
Recent topic of the MU radar is the combination of its radar range-imaging observations of the
turbulence and the direct measurement of the atmospheric parameters by using UAV. Scientists from USA
and France conducted the observation campaign in 2015 and 2016.

G1.5 Equatorial Atmosphere Radar
Equatorial Atmosphere Radar (EAR) is a big atmospheric radar located in West Sumatra, Indonesia.
The EAR was established in June 2001, and has continued long-term observations since June 2001. ResearchInstitute for Sustainable Humanosphere (RISH), Kyoto University and National Institute of Aeronautics andSpace (LAPAN) of Indonesia hold the 15th anniversary ceremony and symposium on August 3, 2016, at

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Jakarta. The ceremony was attended by the Director General for Research and Development, Ministry of
Research, Technology and Higher Education of Indonesia, and Minister/Deputy, Chief of Mission, theEmbassy of Japan in Indonesia and the Minister of the Embassy of Japan. From Kyoto University, Executive
Vice-President for Gender Equality, International Affairs attended. Total number of participants reached 222.
MU radar and EAR web: http://www.rish.kyoto-u.ac.jp/mu+ear/english/index.html

G1.6 Ground-based network observations
MAGDASMAGDAS is the world network of magnetometer developed and maintained by International Center forSpace Weather Science and Education (ICSWSE), Kyushu University. MAGDAS network and its
observations are well maintained during this period. Many studies of atmospheric tides, sudden stratosphericwarming, various ionospheric phenomena, and thermosphere-ionosphere coupling are published ininternational journals. For example, quasi-biennial oscillation is analyzed from Sq current system from thedense magnetometer network over Japan. Also, peak time of equatorial electrojet was deeply investigatedbased on data from the MAGDAS network.
MAGDAS related database web: http://data.icswse.kyushu-u.ac.jp/

VLF/ELF
Institute for Space-Earth Environmental Research (ISEE), Nagoya University reports a campaign
observation of auroras and VLF/ELF waves was carried out from January 28 to February 5, 2014 at Poker
Flat, Alaska, in collaboration with an auroral rocket launch. Dual cameras were used to determine the heightof auroras. A loop antenna with a 20 kHz-sampling portable recorder was tested for VLF/ELF wave
measurement at remote site without power line. They also showed that the first statistical analysis of
ELF/VLF emissions based on 1-year 100 kHz continuous observations at Athabasca, Canada (L = 4.3), in
collaboration with Athabasca University and Kanazawa University. Characteristics of the ELF/VLF
emissions, such as chorus, hiss, and QP emissions, and their dependence on local time, geomagnetic activity,and solar wind parameters are clarified.
ISEE VLF/ELF web: http://stdb2.stelab.nagoya-u.ac.jp/vlf/
AVON (Asia VLF Observation Network) group has been making continuous measurements of
LF/VLF/ELF waves at Tainan (Taiwan), Saraburi (Thailand), Pontianak (Indonesia), Los Banos(Philippines), and Hanoi (Vietnam) since December 2007. 14 Universities/institutes including Chiba,
Hokkaido, Tohoku Universities and Ashikaga Institute of Technology participate in the AVON project. The
antennas consist of a monopole antenna, a dipole antenna, and an orthogonal loop antenna. The sampling
frequency of LF/VLF transmitter signals is 200 kHz, while that of VLF/ELF waves radiated from lightning
discharges is 100 kHz. Recently, the first observation of about 100-s periodic oscillations of intensity andphase in two LF transmitter signals over Japan at 05:52-05:56 UT on March 11, 2011 (about 5’ 42” after themain shock onset the M9.0 earthquake) was reported. The 100-s LF periodic oscillation was caused by thevertical propagation of the acoustic waves excited by the seismic Rayleigh waves. Tohoku University groupis also operating LF/VLF transmitter observation at Ny-Alesund (Norway), Poker Flat (Alaska), Athabasca(Canada), Zhigansk (Russia) to detect energetic electron precipitation from inner magnetosphere. Theseobservations are a part of the ground-based observation networks for the ERG satellite launched on
December 20, 2016.

Airglow imagers
ISEE, Nagoya University is conducting the Optical Mesosphere Thermosphere Imagers (OMTI) in order
to investigate the dynamics of the upper atmosphere through nocturnal airglow emissions. The network is
expanding now and reaches more than 20 stations from the equatorial to the polar regions. Installation of
new instruments during this period was, an imager at Haleakala, Hawaii (March 2013), an imager at Ishigaki(later Yonaguni) (April 2014), an imager at Abuja, Nigeriea (June 2015) and an imager at Eureka, Canada(October 2015). Just recently they also expand the network in northern subauroral region.

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OMTI web: http://stdb2.isee.nagoya-u.ac.jp/omti/

SEALIONSEALION is an ionospheric observation network in Southeast Asia. It has been conducted by National
Institute of Information and Communications Technology (NICT) since 2003 for the purpose of monitoring
and forecasting equatorial ionospheric disturbances, especially plasma bubbles. SEALION is a uniqueionospheric observation network in having the conjugate observational points in the northern and southernhemispheres and around the magnetic equator. The network consists 7 stations in five countries, which are,
Chiang Mai (CMU), Bangkok (KMI), Chumphon (CPN), and Phuket (PKT) in Thailand, Kototabang (KTB)
in Indonesia, Bac Lieu (BCL) in Vietnam, and Cebu (CEB) in Philippines. Observations are FMCW
ionosonde, GPS-TEC, GPS-Scintillation, and Magnetometer.
SEALION data web: http://seg-web.nict.go.jp/sealion/

Planetary atmospheres
Tohoku University and other groups carried out campaign-based large telescope observations ofplanetary atmosphere and ionosphere. Using Subaru/COMICS and IRCS and NASA IRTF/CSHELL, theyreported Jupiter’s infrared aurora and Venus’s cloud characteristics measured by mid-infrared wavelengths(Kasaba et al., 2014, Uno et al., 2014; Sato et al, 2014). They are also operating a 40-cm telescope facility
and a sodium monochromatic imager at the summit of Haleakala, Hawaii to monitor variations in planetaryatmosphere, its surrounding faint gas and its satellite, such as Jupiter’s Io torus and Io’s volcanism, for morethan ten years since 2006 (Yoneda et al., 2014, 2015). They are also operating the large radio telescope(IPRT) at Iitate, Fukushima, and some HF antennas to measure planetary and solar radio emission (Kaneda
et al., 2015; Morioka et al., 2015). Spacecraft data were also used to understand Martian atmosphere, forexample, MGS (Noguchi et al., 2014), Mars Express (Aoki et al., 2014, 2015a, 2015b), and MAVEN (Yigit
et al., 2015, Medvedev et al., 2016). Modeling study was used to understand Jupiter’s atmosphere (Kuroda
et al. 2014) and gravity waves in Martian atmosphere (Haider et al., 2015; Kuroda et al., 2015, 2016).
Haleakala long-term monitoring data web: http://pparc.gp.tohoku.ac.jp/data/hal
IPRT data center web: http://pparc.gp.tohoku.ac.jp/data/iprt/
HF antenna system web: http://ariel.gp.tohoku.ac.jp/jupiter/

G1.7 GNSS receiver network
GEONET (GNSS Earth Observation Network System) is the GPS receiver network over Japan that is
operated by Geospatial Information Authority of Japan (GSI). GEONET consists of 1,300 GPS or morestations. This is one of the largest GNSS network of the world, and the data of every 30s is opened to the
public. GENET web page (in Japanese) is, http://terras.gsi.go.jp/geo_info/geonet_top.html
GEONET is used for the ionospheric study very much. It is well known that Tohoku Earthquake on
March 11, 2011 induced intense ionospheric disturbances, and were clearly observed as fluctuation of GPS
total electron content (TEC). Two-dimensional TEC maps over Japan have been provided routinely by NICT
(http://seg-web.nict.go.jp/GPS/DRAWING-TEC/). One of the prominent research topic related to GEONET
is the real-time three-dimensional ionospheric tomography. This tomography technique uses the constrained
least-squares fitting to reconstruct the electron density distributions. Recently Saito et al. (2016) further
development of the software system enabled to conduct the tomography analysis in the near real-time basis.
They show results of the 3D tomography reconstruction of the ionosphere every 15 minutes with 6 minutes
latency at the following web page: http://www.enri.go.jp/cnspub/tomo3/More application-oriented study is also important with the GNSS use for the ionosphere. ENRI is leading
activities to characterize the spatial gradient in ionospheric TEC for aviation use of GNSS in a frameworkof ICAO (International Civil Aviation Organization) Asia-Pacific region. Ionospheric TEC gradient data4

from States/Administrations in the Asia-Pacific region are being consolidated to develop a “threat model”
for the ground-based augmentation system (GBAS) to enable precise approach guidance for airplanes.

G1.8 Satellite missions
During the period of 2014-2016, there are several satellite missions conducted by JAXA, and used forthe studies of the ionosphere, magnetosphere and planetary sciences.

IMAP/VISI
Airglow emissions at the lower-thermosphere (O2 762 nm, 95km alt.) and the upper-thermosphere (O630 nm, 250 km alt.) are measured with IMAP/VISI on the international space station (ISS) (Akiya et al.,2014). Many concentric gravity wave events in the O2 emission, and equatorial anomaly and plasma bubbles
in O630 nm emission (Perwitasari et al., 2015; Perwitasari et al., 2016). Unfortunately, operation of ISS
IMAP/VISI was terminated by August 2015. Researchers continue analyzing the data from the facility.
IMAP/VISI project web: https://www.iss-imap.org/

AKATSUKIAKATSUKI, also known as the Venus Climate Orbiter (VCO) and Planet-C, is a Japanese (JAXA)
space probe tasked to study the atmosphere of Venus (Sato et al., 2014, 2015). It was launched aboard an HIIA 202 rocket on 20 May 2010. The spacecraft was successfully inserted into the Venus’ orbit by the thrustejection operation on December 7, 2015 (Nakamura et al., 2016). After checking condition of the on-board
instruments, scientific observations started in April 2016, and data analyses are now underway (Ando et al,
2016; Sato et al, 2016).
AKATSUKI mission web: http://www.isas.ac.jp/en/missions/spacecraft/current/akatsuki.html

HISAKIHISAKI, also known as the Spectroscopic Planet Observatory for Recognition of Interaction of
Atmosphere (SPRINT-A), is a Japanese ultraviolet astronomy satellite operated by JAXA (Yamazaki et al.,2014). The first mission of the JAXA’s Small Scientific Satellite program was launched in September 2013
on the maiden flight of the Epsilon rocket. HISAKI carries an extreme ultraviolet spectrometer which will
be used to study the composition of the atmospheres and the behavior of the magnetospheres of the planetsof the Solar System, such as Jupiter (Yoshioka et al., 2014; Yoshikawa et al., 2014, Tao et al., 2016a, 2016b;
Kita et al., 2016; Tsuchiya et al., 2015; Murakami et al., 2016) and Venus (Masunaga et al., 2015).
Campaign-based collaboration with coordinated satellite measurements between Hisaki and Chandra,
XMM-newton, and Hubble Space Telescope were carried out (Kimura et al, 2015, 2016; Badman et al.,2016; Gray et al., 2016; Tao et al., 2016a, 2016b).
HISAKI mission web: http://www.isas.ac.jp/en/missions/spacecraft/current/hisaki.html

ARASE
ARASE, also known as Exploration of energization and Radiation in Geospace (ERG), is a scientific satellite
to study the Van Allen belts. It was developed by the Institute of Space and Astronautical Science of JAXA.
ARASE was launched aboard Epsilon launch vehicle at 11:00:00, 20 December 2016 UTC into apogeeheight 32250 km, perigee 214 km orbit. Subsequent perigee-up operation moved its orbit to apogee 32110
km, perigee 460 km of 565 minutes period (Kasahara et al., 2016). After initial checking for satellite and onboard instruments, JAXA confirmed that every function is working well. Nominal operation has been started
in March 2017, and data analyses and opening are now underway (Kitahara, 2016).
ARASE mission web: http://www.isas.ac.jp/en/missions/spacecraft/current/erg.html

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G1.9 Sounding rocket experiments
Japanese sounding rockets have been used to achieve in-situ measurements in the thermosphere andionosphere as well as other objectives such as microgravity experiment, demonstration of various instrument
and technique, and advanced engineering experiments. In the years of 2014-2016, two rocket experiments
aiming at the ionospheric study were conducted in Japan.
JAXA Sounding Rockets web: http://global.jaxa.jp/projects/rockets/s_rockets/
In August 2014, “S-520-29” sounding rocket experiment was conducted to elucidate three-dimensional
plasma density structure of the sporadic E (Es) layer by using three complemental instruments; opticalimager, radio-wave receiver, and probe for in-situ measurement. Among the onboard instruments, Fast
Langmuir Probe (FLP) successfully measured the electron density and temperature with high time resolution
along the rocket trajectory, and those data were used to understand the detailed structure of electron
temperature inside the Es layer. The result shows that the electron temperature gradually decreases by about
200 K from the outside boundary to the center. Numerical study on the cause of the temperature decrease
was made to find the responsible process.
JAXA Press Release: http://global.jaxa.jp/press/2014/08/20140817_s-520-29.html
In Jan 2016, sounding rocket “S-310-44” equipped with five science instruments was launched from
Uchinoura Space Center to elucidate a mechanism of the ionospheric electron heating in the Sq current focus.
Data from the FLP onboard the rocket suggest that the electron temperature increased by about 200 K withrespect to the background in the altitude range from 100 to 110 km. It is also significant that the observed
energy distribution unlikely seems Maxwellian distribution and sometimes exhibits a possible existence of
non-Maxwellian component in the high electron temperature region. Electron current measured by the fixedbias probe and power spectrum from HF plasma wave receiver indicate that the amplitude in the frequency
range of several hundred Hz significantly increased at the E region altitude. It is remarkable that the strong
electron density perturbation was observed in the broad frequency range from several 100 Hz to 2 kHz at
altitudes from 95 to 110 km.
JAXA Press Release: http://global.jaxa.jp/press/2016/01/20160115_s-310-44.html

G1.10 Instruments for planetary sciences
One of the important research trend during the period 2014-2016 is the enhancement of planetarysciences. Now Japan operates two spacecrafts HISAKI and AKATSUKI for this purpose. Also, researchers
are using number of telescopes on the ground. JAXA recently started the future Mars Moon exploration
project (MMX), which is going to observe Phobos, Deimos and Martian atmosphere, and some groups are
joining in the core teams for science and instruments. Hokkaido University operates 1.6m Pirka Telescopethat is dedicated for observations of planets (http://sana.ep.sci.hokudai.ac.jp/nayoro/index-en.html) (Nakaoet al., 2014). This telescope joins “Optical and Infrared Synergetic Telescope for Education and Research(OISTER)” that networks telescopes of seven universities and National Astronomical Observatory of Japan(NAOJ) (Project web page: http://oister.oao.nao.ac.jp/ (in Japanese)). Tohoku University also plays animportant role to study planets from the ground-based telescope. They were operating a 60-cm telescope
dedicated for planetary observations at Iitate, Fukushima. Unfortunately, the site use was largely limited
because of the nuclear power-plant accident caused by the Tohoku Earthquake in 2011. The facility was thenrelocated to Haleakala in Hawaii in 2014(http://pparc.gp.tohoku.ac.jp/index-en.html). Visible chronagpraph
imager, mid- and high-resolusion Echellle spectrograph (Visp), and super-high resolution heterodyne
spectrograph are installed on T60 (Sakanoi et al., 2014). They are also developing a near-infrared imager
and Echelle spectrograph. Nakagawa et al. (2016) reports results for Venus atmosphere from this facility
after relocation. As shown in the later section (G3.2), the research group is developing a larger facility in thesame location. The study of the planetary atmosphere is a hot topic in the research field. More data fromJapanese satellites and ground-based telescopes are now expected.

6G2. Model and databaseG2.1 GAIA
The demand for quantitative predictions of the situation in the upper atmospheric region has increased,along with brisker human activities in space in recent years. And in conjunction with the effects stemmingfrom human activities, it has become more important to understand the long-term process of atmosphericvariations. Thus, the development of a global atmospheric model is considered beneficial for such demandin the future. In the field of academic research on the upper atmosphere, however, the coupling to the lower
atmosphere has been an essential issue. Evidence regarding the interrelationship between ionospheric andtropospheric variations has been consistently reported based on recent observations using satellites andground-based radars. A model applicable to the entire atmospheric region is thus needed to understand suchvertical coupling from the troposphere through the ionosphere, as variations propagating across regions withdifferent characteristics and complex dynamics must be handled.
The GAIA project combines atmospheric and ionospheric models (developed separately thus far), andtargets the development of a simulation model for the whole global atmosphere. Upon being realized, thismodel will provide a powerful means of studying and solving such upper atmosphere issues as the vertical
coupling in the Earth’s atmosphere. This project is also aimed at reproducing actual upper atmosphericvariations by assimilating observation data into the GAIA model.
Recent achievements with the GAIA model are studies of the sudden stratospheric warming (Pedatella
et al., 2014; 2016; Liu et al, 2014; Miyoshi et al, 2015), global distribution of gravity waves in thethermosphere (Miyoshi et al, 2014), and Weddell Sea Anomaly simulations (Chang et al, 2015).
GAIA project web: http://seg-web.nict.go.jp/GAIA/index_e.html

G2.2 IUGONET
Global phenomena observed in the Earth’s upper atmosphere are the results of many complex processes,
such as the energy and momentum input from the Sun (e.g., solar radiation and solar wind), the energy andmomentum transport by atmospheric waves from the lower atmosphere, and various internal phenomena(e.g., electromagnetic energy transport, plasma convection, chemical reaction). To understand themechanism of the long-term variation in the upper atmosphere, therefore, it is important to analyze various
data (e.g., wind velocity and temperature in the atmosphere, auroral images, geomagnetic field, solar activity
index, etc.) obtained by the global ground-based network observation.
The Inter-university Upper atmosphere Global Observation NETwork (IUGONET) project started in2009 (Abe et al., 2014; Yatagai et al., 2014, 2015). The objective of the project is to establish a metadata
database of various ground-based observation data covering a wide region from the Sun to the Earth; thiswill encourage more studies on the mechanisms of long-term variations in the upper atmosphere. Also, they
developped a software to ease comparison between various types of systems. IUGONET would be importantfor future study of complicated nature of the ionosphere.
Project web: http://www.iugonet.org/?lang=en.

G3. On-going and future plans
G3.1 Masterplan / Roadmap 2014 and 2017
Research Institute for Sustainable Humanosphere (RISH), Kyoto University, National Institute of Polar
Research (NIPR), Institute for Space-Earth Environmental Research (ISEE), Nagoya University, andInternational Center for Space Weather Science and Education (ICSWSE), Kyushu University proposed theresearch project “Coupling process in the solar-terrestrial system” to Masterplan 2017 of Science Council ofJapan. This is a project to study the solar energy inputs into the Earth, and the response of Geospace(magnetosphere, ionosphere and atmosphere) to the energy input. We plan to install large atmospheric radars
with active phased array antenna at the equator and the Arctic regions. One is Equatorial MU (EMU) radar
by RISH in Sumatera Island, Indonesia, and the other is EISCAT_3D by NIPR in northern Scandinavia
under international collaborations. We develop the global observation network (ISEE, ICSWSE with otherinstitutions). The participating institutions have already started budget request of their facilities. The same7

project was once proposed to Masterplan 2014, and was approved as one of 27 high-priority projects, andfurther approved as one of 11 new plans in the Roadmap 2014 of Ministry of Education, Culture, Sports,
Science and Technology (MEXT). We continue to pursue realization of this research project.
Project web: http://www.rish.kyoto-u.ac.jp/masterplan2017/index-e.html

G3.2 Telescope PLANETS“PLANETS” is a project to develop a new telescope dedicated to the planetary science by theinternational collaboration by University of Hawai'i Institute for Astronomy (IfA), Tohoku University, andthe Kiepenheuer Institute for Solar Physics (KIS) and the National Autonomous Univesity of Mexico(UNAM). The telescope has a low-scattering optical system with a 1.8m-diameter off-axis main mirror toobserve faint emission near a bright object, such as resonant/Rayleigh/Mie scattering surrounding aplanet/satellite. Off-axis telescopes can have far superior contrast because there are no obstructions in the
beam such as secondary mirror supports. This limits the diffraction as well as scattered light from
obstructions. The telescope would also be highly polished to minimize diffuse scatter from mirror roughness- a major source of scattering at large angles. The project is now underway, and expects the first light inearly 2018.
Project web: https://www.planets.life/planets-telescope/G3.3 SMILES-2
The Effectiveness of highly sensitive submillimeter-wave limb sounder in vertical-distribution
measurements of atmospheric chemical compositions, temperature, and wind over a wide altitude range has
been demonstrated by the Superconducting Submillimeter-wave Limb-Emission Sounder (SMILES), which
was operated in 2009-2010 winter on the International Space Station. A new proposal is being put out as
SMILES-2, which is a satellite mission carrying submillimeter-wave limb sounder inherited from SMILES.
When realized, SMILES-2 will provide precise measurement of vertical distribution of compositions,temperature, and wind, in an extend altitude by implementing multi-frequency band receiver including THz
channel (Baron et al, 2015; Suzuki et al., 2015).
SMILES web: http://smiles.tksc.jaxa.jp/about/index_e.html
SMILES-2 conceptual design: https://repository.exst.jaxa.jp/dspace/handle/a-is/609876?locale=en

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