ARC-Space (Aizu Research Cluster for Space Science)
ARC-Space publicized new findings on composition of lunar crust which had been obtained from data provided by the lunar orbiter “Kaguya” and concluded an agreement with Japan Aerospace Exploration Agency (JAXA) regarding development of human resources in the aerospace field.
ARC-Environment (Aizu Research Cluster for Environmental Informatics)
ARC-Environment developed a high-resolution weather forecasting system for the areas in Fukushima Prefecture, and has been worked on development of a system to distribute weather information via the Web in collaboration with local companies.
ARC-Medical (Aizu Research Cluster for Medical Engineering and Informatics)
ARC-Medical participated in the MEXT-supported program, “Regional Innovation Cluster Program (Category: Prioritized Support)”, with Fukushima Medical University as a representative, and assisted development of medical devices in term of information technology.
Y. Ogawa, T. Matsunaga, R. Nakamura, K. Saiki, M. Ohtake, T. Hiroi, H. Takeda, T. Arai, Y. Yokota, S. Yamamoto, N. Hirata, T. Sugihara, S. Sasaki, J. Haruyama, T. Morota, C. Honda, H. Demura, K. Kitazato, J. Terazono, and N. Asada. The widespread occurrence of high-calcium pyroxene in bright-ray craters on the Moon and implications for lunar-crust composition. Geophysical Research Letters, 38:L17202, 2011.
We investigated the continuous spectral features of fresh craters on the Moon accompanied by distinctive bright rays, with cavity diameters between 8 and 24 km. We used the data from the Spectral Profiler onboard SELENE (Kaguya) to gain a better understanding of the composition of the lunar highland crust. We found that the observed spectra exhibited strong symmetric absorption around 1 spectra exhibited strong symmetric absorption around 1 μm and recognizable absorption around 1.3 μm. The spectra around a few craters showed a drastic change in the relative strengths of these two absorption bands s1.3/1.0 at different locations in and around the craters, indicating differences in the abundance of plagioclase and mafic minerals. In contrast, the spectra around most of the craters showed no significant variation in spectral shape, with an essentially constant s1.3/1.0. We analyzed the absorption features of the craters with an essentially constant s1.3/1.0 using the Modified Gaussian Model. We found that the strongest symmetric absorption bands were centered at 0.97-1.01 μm with s1.3/1.0 ≈ 0.2-0.6. Comparing these values with data from known samples, we concluded that high-calcium pyroxene (HCP) is the most plausible dominant mafic mineral identified from the observed spectra. The fact that we detected such HCP-dominant spectra among rayed craters widely spaced across the lunar highland implies that the major mafic component of some portions of the lunar crust is HCP rather than low-calcium pyroxene (LCP).
Y. Yokota, T. Matsunaga, M. Ohtake, J. Haruyama, R. Nakamura, S. Yamamoto, Y. Ogawa, T. Morota, C. Honda, K. Saiki, K. Nagasawa, K. Kitazato, S. Sasaki, A. Iwasaki, H. Demura, N. Hirata, T. Hiroi, R. Honda, Y. Iijima, and H. Mizutani. Lunar photometric properties at wavelengths 0.5-1.6 H. Mizutani. Lunar photometric properties at wavelengths 0.5-1.6 ?m m acquired by SELENE Spectral Profiler and their dependency on local albedo and latitudinal zones. Icarus, 215:639-660, 2011.
The lunar photometric function, which describes the dependency of the observed radiance on the observation geometry, is used for photometric correction of lunar visible/near-infrared data. A precise photometric correction parameter set is crucial for many applications including mineral identification and reflectance map mosaics. We present, for the first time, spectrally continuous photometric correction parameters for both sides of the Moon for wavelengths in the range 0.5-1.6 μm and solar phase angles between 5° and 85°, derived from Kaguya (SELENE) Spectral Profiler (SP) data. Since the measured radiance also depends on the surface albedo, we developed a statistical method for selecting areas with relatively uniform albedos from a nearly 7000-orbit SP data set. Using the selected data set, we obtained empirical photometric correction parameter sets for three albedo groups (high, medium, and low). We did this because the photometric function depends on the albedo, especially at phase angles below about 20° for which the shadow hiding opposition effect is appreciable. We determined the parameters in 160 bands and discovered a small variation in the opposition effect due to the albedo variation of mafic mineral absorption. The consistency of the photometric correction was checked by comparing observations made at different times of the same area on the lunar surface. Variations in the spectra obtained were lower than 2%, except for the large phase angle data in mare. Lastly, we developed a correction method for low solar elevation data, which is required for high latitude regions. By investigating low solar elevation data, we introduced an additional correction method. We used the new photometric correction to generate a 1° mesh global lunar reflectance map cube in a wavelength range of 0.5-1.6 μm. Surprisingly, these maps reveal that high latitude (≥ 75°) regions in both the north and south have much lower spectral continuum slopes (color ratio r1547.7nm/r752.8nm ≤ 1.8) than the low and medium latitude regions, which implies lower degrees of space weathering.
J. Kimura, T. Kawamura, H. Morito, T. Morota, C. Honda, K. Kuramoto, and T. Okada. Sublimation's impact on temporal change of albedo dichotomy on Iapetus. Icarus, 214:596-605, 2011.
Iapetus, one of the Saturnian moons, has an extreme albedo contrast between the leading and trailing hemispheres. The origin of this albedo dichotomy has led to several hypotheses, however it remains controversial. To clarify the origin of the dichotomy, the key approach is to investigate the detailed distribution of the dark material. Recent studies of impact craters and surface temperature from Cassini spacecraft data implied that sublimation of H2O ice can occur on Iapetus’surface. This ice sublimation can change the albedo distribution on the moon with time. In this study, we evaluate the effect of ice sublimation and simulate the temporal change of surface albedo. We assume the dark material and the bright ice on the surface to be uniformly mixed with a certain volume fraction, and the initial albedo distribution to incorporate the dark material deposits on the surface. That is, the albedo at the apex is lowest and concentrically increases in a sinusoidal pattern. This situation simulates that dark materials existed around the Iapetus’orbit billions of years ago, and the synchronously rotating Iapetus swept the material and then deposited it on its surface. The evolution of the surface albedo during 4.0 Gyr is simulated by estimating the surface temperature from the insolation energy on Iapetus including the effect of Saturn’s eccentricity and Iapetus’obliquity precession, and evaluating the sublimation rate of H2O ice from the Iapetus’surface. As a result, we found that the distribution of the surface albedo changed dramatically after 4.0 Gyr of evolution. The sublimation has three important effects on the resultant surface albedo. First, the albedo in the leading hemisphere has significantly decreased to approach the minimum value. Second, the albedo distribution has been elongated along the equator. Third, the edge of the low albedo region has become clear. Considering the effect of ice sublimation, the current albedo distribution can be reconstructed from the sinusoidal albedo distribution, suggest the apexan tapex cratering asymmetry as a candidate for the origin of the albedo dichotomy. From the model analysis, we obtained an important aspect that the depth of the turn-over layer where the darkening process proceeded for 4 Gyr should be an order of 10 cm, which is consistent with evaluation from the Cassini radar observations.
S. Yamamoto, T. Matsunaga, Y. Ogawa, R. Nakamura, Y. Yokota, M. Ohtake, J. Haruyama, T. Morota, C. Honda, T. Hiroi, and S. Kodama. Preflight and In-Flight Calibration of the Spectral Profiler on Board SELENE (Kaguya). IEEE Transactions on Geoscience and Remote Sensing, 49:4660-4676, 2011.
The Spectral Profiler (SP) is a visible-near infrared spectrometer on board the Japanese Selenological and Engineering Explorer, which was launched in 2007 and observed the Moon until June 2009. The SP consists of two gratings and three lineararray detectors: VIS (0.5-1.0 μm), NIR 1 (0.9-1.7 μm), and NIR 2 (1.7-2.6 μm). In this paper, we characterize the radiometric and spectral properties of VIS and NIR 1 using in-flight observational data as well as preflight data derived in laboratory experiments using a calibrated integrating sphere. We also proposed new methods for radiometric calibration, specifically methods for nonlinearity correction, wavelength correction, and the correction of the radiometric calibration coefficients affected by the water vapor. After all the corrections, including the photometric correction, we obtained the reflectance spectra for the lunar surface. Finally, we examined the stability of the SP using the SP data near the Apollo 16 landing site observed at four different times. The difference in reflectance among these four observations was less than ±1% for most of the bands, suggesting that the degradation of the SP is not significant over the mission period.
S. Urakawa, S. Okumura, K. Nishiyama, T. Sakamoto, N. Takahashi, S. Abe, M. Ishiguro, K. Kitazato, D. Kuroda, S. Hasegawa, K. Ohta, N. Kawai, Y. Shimizu, S. Nagayama, K. Yanagisawa, M. Yoshida, and M. Yoshikawa. Photometric observations of 107P/Wilson-Harrington. Icarus, 215(1):17-26, 2011.
We present lightcurve observations and multiband photometry for 107P/WilsonHarrington using five small- and medium-sized telescopes. The lightcurve has shown a periodicity of 0.2979 day (7.15 hour) and 0.0993 day (2.38 hour), which has a commensurability of 3:1. The physical properties of the lightcurve indicate two models: (1) 107P/Wilson-Harrington is a tumbling object with a sidereal rotation period of 0.2979 day and a precession period of 0.0993 day. The shape has a long axis mode (LAM) of L1:L2:L3 = 1.0:1.0:1.6. The direction of the total rotational angular momentum is around λ = 310°, Β = −10°, or λ = 132°, Β = −17°. The nutation angle is approximately constant at 65°. (2) 107P/Wilson-Harrington is not a tumbler. The sidereal rotation period is 0.2979 day. The shape is nearly spherical but slightly hexagonal with a short axis mode (SAM) of L1:L2:L3 = 1.5:1.5:1.0. The pole orientation is around λ = 330°, Β = −27°. In addition, the model includes the possibility of binary hosting. For both models, the sense of rotation is retrograde. Furthermore, multiband photometry indicates that the taxonomy class of 107P/Wilson-Harrington is C-type. No clear rotational color variations are confirmed on the surface.
Y. M. Min, V. N. Kryjov, K. H. An, S. N. Hameed, S. J. Sohn, W. J. Lee, and J. H. Oh. Evaluation of the weather generator CLIGEN with daily precipitation characterisitics in Korea. Asia Pacific Journal of Atmospheric Sciences, 46(3):255-263, 2011.
The ability of the CLImate GENerator (CLIGEN) weather generator to reproduce daily precipitation characteristics for Korea was assessed on the basis of 55-year long historical daily precipitation records from eight weather stations (Seoul, Incheon, Daegu, Ulsan, Gwangju, Busan, Kangneung, and Jeonju) representing different parts of the Korean peninsula. The basic statistics of daily precipitation (mean, standard deviation, skewness of daily precipitation, number of rainy days, and the lengths of wet/dry period), probability distribution characteristics of daily precipitation (percentiles and maximum value), and the spatial covariance statistic generated by CLIGEN were compared with those derived from the observed weather series. Significance tests were conducted on the difference between the historical and generated statistics with the 1% significance level. The results show that CLIGEN simulates most of the daily precipitation characteristics satisfactorily with a tendency to slightly underestimate the mean and variability of daily precipitation. Especially, the number of rainy days is perfectly reproduced with mean relative error of 0.4% across all the stations. It is also found that the spatial covariance statistic from eight different stations is well reproduced by CLIGEN with respect to the leading EOF mode of summer season daily precipitation.
S. Yamamoto, R. Nakamura, T. Matsunaga, Y. Ogawa, Y. Ishihara, T. Morota, N. Hirata, M. Ohtake ant T. Hiroi, Y. Yokota, and J. Haruyama. Olivine-rich exposures in the South Pole-Aitken Basin. Icarus, 218:331-344, doi: 10.1016/j.icarus.2011.12.012, March 2012.
The distribution and the geological context of the olivine-rich exposures in the South Pole-Aitken (SPA) Basin on the Moon were investigated based on the spectral data obtained from the Spectral Profiler (SP) and Multiband Imager (MI) onboard the Japanese lunar explorer Kaguya/SELENE. The olivine-rich exposures are found only in the peak rings or central peaks of the Schrodinger basin and Zeeman crater, which are located in the outer region of the SPA Basin and not in the center region. On a localized scale, the olivine-rich materials are exposed on landslide features on the crater walls or sloped wall of the central peaks or the peak rings. Another observational finding is the co-existence of olivine-rich and plagioclase-rich materials on a kilometer scale spanning most of the olivine-rich sites in the Schrodinger basin. Pyroxene-rich materials are found in fresh craters outside the peak rings or the central peaks with olivine-rich materials. Based on these results, the following scenario are proposed: (1) the impact to form the SPA Basin melted a large amount of the lunar upper mantle and crust, and distributed the melted materials to the outer region; (2) local differentiation of melted materials hid the olivine-rich materials in the center region of the SPA Basin; (3) later impacts that formed the Schrodinger and Zeeman craters excavated and exposed the olivine-rich materials to the surface again; and (4) space weathering and regolith gardening obscured the olivine-rich spectra at the exposure sites, but recent, small scale impacts or landslides on the sloped wall exposed fresh olivine-rich materials, allowing the identification of the olivine-rich exposures by spectral remote-sensing. This suggests that several, different scale events play an important role in forming the surface distributions of originally deep-seated materials on the Moon, as well as on other planetary bodies.
Y. Takagi, M. Yoshikawa, M. Abe, S. Tachibana, T. Okada, K. Kitazato, R. Nakamura, N. Hirata, H. Yano, H. Demura, S. Nakazawa, Y. Iijima, K. Shirai, and M. Hayakawa. Hayabusa2, C-type asteroid sample return mission. In American Geophysical Union, Fall Meeting 2011, number P21E-04, December 2011.
Asteroid Explorer "Hayabusa2" is a successor of "Hayabusa" (MUSES-C), which revealed several new technologies and returned to Earth in June 2010. While establishing a new navigation method using ion engines, Hayabusa brought back samples from the asteroid "Itokawa" to help elucidate the origin of the solar system. Hayabusa2 will target a C-type asteroid "1999 JU3" to study the origin and evolution of the solar system as well as materials for life by leveraging the experience acquired from the Hayabusa mission. To learn more about the origin and evolution of the solar system, it is important to investigate typical types of asteroids, namely S-, C-, and D-type asteroids. A C-type asteroid, which is a target of Hayabusa2, is a more primordial body than Itokawa, which is an S-type asteroid, and is considered to contain more organic or hydrated minerals although both S- and C- types have lithologic characteristics. Minerals and seawater which form the Earth as well as materials for life are believed to be strongly connected in the primitive solar nebula in the early solar system, thus we expect to clarify the origin of life by analyzing samples acquired from a primordial celestial body such as a C-type asteroid to study organic matter and water in the solar system and how they coexist while affecting each other. Hayabusa2 will utilize new technology while further confirming the deep space round-trip exploration technology by inheriting and improving the already verified knowhow established by Hayabusa to construct the basis for future deep-space exploration. The configuration of Hayabusa2 is basically the same as that of Hayabusa, but we will modify some parts by introducing novel technologies that evolved after the Hayabusa era. For example, the antenna for Hayabusa was in a parabolic shape, but the one for Hayabusa2 will be flattened. Also, a new function, "collision device", is considered to be onboard to create a crater artificially. An artificial crater that can be created by the device is expected to be a small one with a few meters in diameter, but still, by acquiring samples from the surface that is exposed by a collision, we can get fresh samples that are less weathered by the space environment or heat. Hayabusa2 is scheduled for launch in 2014 (or 2015 as a backup.) It should arrive at the C-type asteroid in mid 2018, staying around there for one and half years before leaving the asteroid at the end of 2019 and returning to Earth around the end of 2020.
S. N. Hameed and Y. S. Shen. On a Tropical Southern Mode of Oscilla tion at Intraseasonal Timescales. In 8th Annual meeting of the Asia Oceania Geosciences Society, page 96. AOGS, August 2011.
Spectral analysis of Outgoing Longwave Radiation (OLR) over the tropical Indian Ocean revealed spatially and spectrally distinct modes of boreal winter time variability within the intraseasonal timescales. The first mode, exhibited marked equatorial symmetry and occupied a 30-40 day band in the spectra. The second mode had a distinct peak and occupied a 50-70 day band, while exhibiting strongly asymmetric variability south of the equator in the central Indian Ocean. In this presentation, we substantiate this finding with alternate analysis and discuss the two modes in greater detail. The differential role of these modes in modulating interannual events such as ENSO and IOD is investigated.
M. Ohtake, T. Mastunaga, H. Takeda, Y. Yokota, S. Yamamoto, T. Morota, Y. Ishihara, Y. Ogawa, T. Hirori, R. Nakamura, and J. Haruyama. Compositional trend within the lunar highland crust. In EPSC-DPS Joint Meeting 2011, page 802, October 2011.
In this study we investigated spatial and vertical compositional (modal abundance) trends of the high plagioclase abundance anorthosite rocks over the entire lunar surface within the upper crust by using continuous reflectance spectra derived by the SELENE Spectral Profiler (SP) and images derived by the SELENE Multiband Imager (MI). We also investigated compositional trend within the deeper area than a central peak excavation depth (possibly lower crust) based on a composition of Orientale ejecta. Orientale is selected because it is young and least disturbed by later impact event.
T. Okada, T. Fukuhara, S. Tanaka, M. Taguchi, R. Nakamura, T. Sekiguchi, S. Hasegawa, Y. Ogawa, K. Kitazato, T. Matsunaga, T. Imamura, T. Wada, T. Arai, Y. Yamamoto, R. Takaki, S. Tachikawa, J. Helber, and T. G. Mueller. Thermal Infrared Imager TIR on Hayabusa 2 to Investigate Physical Properties of C-Class Near-Earth Asteroid 1999JU3,. In 43rd Lunar and Planetary Science Conference, pages No. 1659, id.1498, March 2012.
Thermal-infrared imager TIR is being prepared to observe a C-class ENA 1999JU3 in Hayabusa 2, not only for scientific investigation of asteroid physical properties but also for landing site selection and safety descent to asteroid surface.
M. Ohtake, H. Takeda, T. Mastunaga, Y. Yokota, J. Haruyama, T. Morota, S. Yamamoto, Y. Ogawa, T. Hiroi, Y. Karouji, K. Saiki, and P. G. Lucey. Primitive Farside Highland Materials Detected by Mg Number. In 43rd Lunar and Planetary Science Conference, pages No. 1659, id.1977, March 2012.
We utilize a new algorithm that derives Mg-number from spectral reflectance data to derive a global map of Mg-number. The derived Mg-number distribution of the lunar highlands clearly indicates its dichotomic distribution, with a higher Mg-number in the farside highlands than in the nearside.
Y. Ogawa, J. Haruyama, T. Matsunaga, R. Nakamura, T. Morota, T. Hiroi, Y. Yokota, S. Yamamoto, S. Sasaki, M. Ohtake, C. Honda, H. Demura, and J. Terazono. Spectral analysis of Reiner Gamma on the Moon using the data from Spectral Profiler onboard SELENE/Kaguya. In EPSCDPS Joint Meeting 2011, page 625, October 2011.
Space weathering causes the change in optical properties, such as darkening, reddening, and decrease of absorption depths of the planetary surfaces. Two competing processes have been proposed so far as the main mechanism of such space weathering; hydrogen irradiation by solar wind and bombardment of micrometeorites. We use the new data set obtained by Spectral Profiler (SP) onboard SELENE/Kaguya which observed the Moon and approach the actual process of space weathering on the Moon.
Y. Yokota, T. Matsunaga, S. Yamamoto, M. M. Ohtake, J. Haruyama, R. Nakamura, Y. Ogawa, T. Morota, C. Honda, K. Saiki, K. Nagasawa, K. Kitazato, S. Sasaki, A. Iwasaki, H. H. Demura, N. Hirata, T. Hiroi, R. Honda, Y. Iijima, and H. Mizutani. Lunar Photometric Properties at Wavelength over 1.7 Microns Acquired by SELENE Spectral Profiler NIR-2 Sensor. In 43rd Lunar and Planetary Science Conference, pages No. 1659, id.2810, March 2012.
We present photometric correction method for SELENE SP NIR-2 sensor.
S. Yamamoto, R. Nakamura, T. Matsunaga, Y. Ogawa, Y. Ishihara, T. Morota, N. Hirata, M. Ohtake, T. Hiroi, Y. Yokota, and J. Haruyama. Global Distribution Trend of Purest Anorthosite on the Moon Revealed by SELENE Spectral Profiler. In 43rd Lunar and Planetary Science Conference, pages No. 1659, id.1356, March 2012.
We report the global distribution trend and the modes of occurrence of purest anorthosite (PAN) on the Moon revealed by the Spectral Profiler onboard the Japanese lunar explorer SELENE (Kaguya).
Y. Ogawa, J. Haruyama, T. Matsunaga, R. Nakamura, T. Morota, T. Hiroi, Y. Yokota, S. Yamamoto, S. Sasaki, M. Ohtake, C. Honda, and H. Demura. Spectral analysis of lunar swirls using the data from Spectral Profiler onboard SELENE/Kaguya. In American Geophysical Union Fall Meeting 2011, pages P13D1702, December 2011.
Space weathering causes the change in optical properties, such as darkening, reddening, and decrease of absorption depths of the planetary surfaces. Two competing processes have been proposed so far as the main mechanism of such space weathering; hydrogen irradiation by solar wind and bombardment of micrometeorites. We used the new data set obtained by Spectral Profiler (SP) onboard SELENE/Kaguya which observed the Moon and investigated the optical properties of the representative lunar swirls. We searched for any systematic relationship between the albedo and the maturity, which are represented by the (1) reflectance at 0.75 micron (r0.75) and slopes of the fitted continua or (2) r0.75 and depth/strength of absorption band of 1 micron and 1.3 micron, respectively. Based on the results of our spectral analyses including MGM (Modified Gaussian Model), we try to approach the actual process of space weathering on the Moon.
J. Terazono, R. Nakamura, S. Kodama, N. Yamamoto, H. Demura, N. Hirata, Y. Ogawa, and T. Sugawara. WISE-CAPS: Archiving, Browsing and Analyzing Environment for Lunar and Planetary Data: Current Enhancement and Future Prospect. In 43rd Lunar and Planetary Science Conference, pages No. 1659, id.1198, March 2012.
This presentation describes current enhancement and future prospects on our webGIS-based archiving, browsing, and analyzing environment of lunar and planetary data, called WISE-CAPS, including integrated data display and data uploading mechanism.
C. Honda, S. Suzuki, N. Hirata, T. Morota, H. Demura, M. Ohtake, J. Haruyama, and N. Asada. Retention time of crater ray materials on the lunar highland. In EPSC-DPS Joint Meeting 2011, October 2011.
T. Kinoshita, C. Honda, N. Hirata, T. Morota, H. Demura, and N. Asada. Evaluation of spatial distribution of craters on lunar surface for detection of secondary craters. In 43rd Lunar and Planetary Science Conference, March 2012.
K. Saiki, T. Arai, H. Araki, Y. Ishihara, M. Ohtake, K. Yuzuru, N. Kobayashi, T. Sugihara, J. Haruyama, C. Honda, and H. Sato. Landing Site Evaluation for the Next Lunar Exploration Project: SELENE-2. In American Geophysical Union, Fall Meeting 2011, December 2011.
Y. Ogawa, J. Haruyama, T. Matsunaga, R. Nakamura, T. Morota, T. Hiroi, Y. Yokota, S. Yamamoto, S. Sasaki, M. Ohtake a nd C. Honda, H. Demura, and J. Terazono. Spectral analysis of Reiner Gamma on the Moon using the data from Spectral Profiler onboard SELENE/Kaguya. In EPSC-DPS Joint Meeting 2011, October 2011.
Y. Yokota, T. Matsunaga, S. Yamamoto, M. Ohtake, J. Haruyama, R. Nakamura, Y. Ogawa, T. Morota, C. Honda, K. Saiki, K. Nagasawa, K. Kitazato, S. Sasaki, A. Iwasaki, H. Demura, N. Hirata, T. Hiroi, R. Honda, Y. Iijima, and H. Mizutani. Landing Site Evaluation for the Next Lunar Exploration Project: SELENE-2. In 43rd Lunar and Planetary Science Conference, March 2012.
Y. Ogawa, J. Haruyama, T. Matsunaga, R. Nakamura, T. Morota, T. Hiroi, Y. Yokota, S. Yamamoto, S. Sasaki, M. Ohtake, C. Honda, and H. Demura. Spectral analysis of lunar swirls using the data from Spectral Profiler onboard SELENE/Kaguya. In American Geophysical Union, Fall Meeting 2011, December 2011.
C. Honda, S. Suzuki, N. Hirata, T. Morota, H. Demura, M. Ohtake, J. Haruyama, and N. Asada. Retention time of crater ray materials on the Moon. In American Geophysical Union, Fall Meeting 2011, December 2011.
C. Honda. JSPS Grant-in-Aid for Young Scientists (B) 2011-2012.
S. N. Hameed. Extending APEC Climate Center Seasonal Forecast and Climate Adaptation products for improved societal applications, 2011.
R. Yoshioka, Y. Watanobe, H. Terasaka and N. N. Mirenkov. Research and development of self-explanatory programming language for nuclear energy safety analysis , Japanese Nuclear Energy Safety, 2011.
Y. Ogawa. JSPS Grant-in-Aid for Young Scientists (B) 2011.
T. Sampe, November 2011.
'Yamamoto-Syono award for outstanding papers' was awarded from the Meteorological Society of Japan
Y. Ogawa, April 2011.
Regular member, The Japanese Society for Planetary Sciences
Y. Ogawa, April 2011.
Regular member, American Geophyisical Union
Y. Ogawa, April 2011.
Committee member of JGU gender equality Ph.D, Master and Graduation Theses
Narumi Ishige. Graduation thesis, School of Computer Science and Engineering, 2012.
Thesis Adviser: T. Sampe
Shuhei Ikari. Graduation thesis, School of Computer Science and Engineering, 2012.
Thesis Adviser: T. Sampe
Hikaru Ishikawa. Graduation thesis, School of Computer Science and Engineering, 2012.
Thesis Adviser: T. Sampe