Curriculum Vitaes

Yoshitaka Saito

  (斎藤 芳隆)

Profile Information

Affiliation
Associate Professor, Institute of Space and Astronautical Science, Department of Interdisciplinary Space Science, Japan Aerospace Exploration Agency
Degree
(BLANK)(The University of Tokyo)
(BLANK)(The University of Tokyo)

J-GLOBAL ID
200901068528199528
researchmap Member ID
1000227990

科学観測用気球の開発とそれを用いた科学観測を行っています。気球には到達できる高さ、飛翔時間の制限がありますが、それを大きく打ち破る気球が誕生しつつあります。気球の研究を進め、気球の可能性を広げ、様々な科学観測実験で利用できるようにしたいと考えています。

 修士過程では、所属する研究室で開発が進められていた天体硬X線検出器を用いた気球実験に携わりました。博士過程ではそれを将来のX線天文衛星搭載用に発展させると共に、X線天文衛星「あすか」による回転駆動型パルサーの観測を行い、エネルギー放射機構の研究を進めました。

 その後、宇宙研気球グループに奉職し、高エネルギー宇宙物理に関する観測実験を継続すると共に、気球本体、搭載機器、地上系といった気球実験システム全般の開発と運用に従事するようになりました。気球の飛翔実験実施にあたっては受信班として、気球と地上間のデータ伝送の確立を担っています。

 気球本体の開発として最初に手掛けたのは、薄い皮膜を開発し、それを用いた気球を開発することで、飛翔高度を向上させる研究でした。3.4 um厚のフィルムを開発し、2002年にはそのフィルムを用いた気球により30年ぶりに世界最高気球高度記録を更新しています。さらにより薄いフィルムの開発を進め、2013年には2.8 um厚のフィルムにより、再度の記録更新に成功しました。

 この研究と並行して進めているのがスーパープレッシャー気球の開発です。これは、気球を密閉して加圧することで、夜間の浮力の低下を防ぎ、長時間の飛翔を可能にする気球です。2000年代は気球皮膜自体の開発や、ロープと皮膜を組み合わせることで構造強度を向上させたLobed-pumpkin型やその展開性能を改善した俵型の気球の開発を進めました。2010年には皮膜に菱形の目の網をかぶせることで軽い構造で高い耐圧性能が得られることを見出し、以後、この型の気球の開発を進めております。スーパープレッシャー気球の実現には、軽い構造で十分な耐圧性能と気密性能を持たせることが大切です。2019年には体積6,400 m3の気球の地上試験(地上試験としては世界最大級です)を実施し、十分な安全率をもって、高度27 kmに70 kgのペイロードを長時間飛翔させることができる耐圧性能を有することを確認しました。2020年には体積2,000 m3の気球の飛翔試験を実施したのですが、放球直後からガス漏れが発生するという不具合が発生しました。放球時に網が叩いたことで皮膜が衝撃破壊を起こしたもので、これを防ぐべく、2020~2023年にかけて、準静的に気球を立ち上げて放球する新しい方法を開発し、その実証試験まで完了しました。2024年には、この放球方法により、再度、体積2,000 m3の気球の飛翔試験を実施する計画です。また、皮膜を多層化することで10日以上の飛翔が可能となる気密性能が得られること、耐圧性能は3,000 Paを超えることを体積180 m3の小型気球の地上試験で実証しました。2022年には、この型の気球を用いて、南極域での大気重力波観測が実施され、2024年には改良を加えた気球での実験を計画しています。

満膨張になった体積6,400 m3の気球

 このように、気球の研究は進んでいるのですが、一方で、気球を用いた科学観測実験の方は開店休業状態であり、これが実施できていないことには忸怩たる思いがあります。残念ながら、現状の我が国の気球実験システムでは、気球の飛翔期間が数10時間に限られてしまうため、得られる光子数が乏しく、実施したい高エネルギー天体の研究が困難なのです。むろん、この制限の元で科学的な成果をあげることも不可能ではありませんが、自分が我が国で唯一、大気球の飛翔機会を提供している研究所に所属し、我々以外に気球の研究を進めているグループが存在しない現状を考えると、気球を用いた実験を実施するよりも、気球の研究を推進し、自らの実験を可能にすると共に、みなさまに利用していただける気球が提供できるようにすることこそが責務、と感じております。

 長時間飛翔が可能な気球は世界的にも黎明期にあり、我が国ではその技術は未獲得です。大型気球は開発コストが嵩むため、小型気球からの開発となるのですが、技術的には小型の方が困難です。これは、気球重量が表面積に比例しているのに対し、浮力は体積に比例することが一因で、もう一つには気球皮膜の欠陥数は表面積に比例するのに対し、ガス漏れの許容量は気球体積に比例するためです。上にも記載しましたが、我々は耐圧性能、気密性能、それぞれの向上手段を見出しており、これらを用いて科学観測に利用できる気球を開発し、小型気球による科学観測を開始したいと考えています。 


Papers

 305
  • J. P. Wefel, S. Torii, Y. Shimizu, K. Kasahara, N. Hasebe, M. Hareyama, S. Kodaira, O. Okudaira, N. Yamashita, M. Miyazima, T. Miyaji, M. Tkayanagi, S. Ueno, H. Tomida, Y. Saito, H. Fuke, T. Yamagami, J. Nishimura, T. Tamura, N. Tateyama, K. Hibino, S. Okuno, A. Shiomi, M. Takita, T. Yuda, F. Kakimoto, Y. Tsunesada, T. Terasawa, T. Kobayashi, A. Yoshida, K. Yamaoka, Y. Katayose, M. Shibata, M. Ichimura, S. Kuramata, Y. Uchihori, A. Kitamura, K. Yoshida, H. Murakami, Y. Komor, K. MIZUTANl, K. Munakata, R. E. Streitmatter, J. W. Mitchell, L. M. BARBlER, A. A. MOlSEEV, J. F. Krizmanic, J. F. Ormes, G. Case, M. L. Cherry, T. G. Guzik, J. B. Isbert, W. R. Binns, M. H. Israel, H. S. Krawczynski, P. S. Marrocchesi, G. Bigongiari, K. Batkov, M. Y. Kim, M. G. Bagliesi, P. Masestro, V. Millucci, R. Zei, O. Adriani, P. Papini, E. Vannuccini, L. Bonechi, J. Chang, J. Yan, W. Gan, G. Chen, Y. Ma, H. Wang
    Astroparticle, Particle and Space Physics, Detectors and Medical Physics Applications - Proceedings of the 10th Conference, 911-915, 2008  Peer-reviewed
    The CALorimetric Electron Telescope, CALET, is a new Space Observatory being developed for the Japanese Experiment Module Exposed Facility, JEM-EF, of the International Space Station. Major scientific objectives are to search for nearby cosmic ray sources and dark matter by carrying out a precise measurement of the electron spectrum from 10's of GeV-10 TeV and of gamma rays in the range 20 MeV several TeV. CALET has a unique capability to observe electrons and y-rays over 1 TeV, with a hadron rejection power better than 105 and an energy resolution of a few % beyond 100 GeV. Moreover, CALET will follow PAMELA, GLAST and other experiments and can both extend and refine the observations made by those missions. The main instrument, to be described, consists of an imaging calorimeter combined with a total absorption calorimeter. With auxiliary detectors, the CALET Observatory will also monitor solar activity and study pray bursts. The phase NB study is underway for a proposed 2013 launch on the H-I1 Transfer Vehicle (HTV) for 3- 5 years of observation on EM-EF.
  • Y. Kishimoto, S. Gunji, Y. Ishikawa, M. Takada, N. Toukairin, Y. Tanaka, F. Tokanai, H. Sakurai, T. Mihara, T. Sato, K. Hayashida, N. Anabuki, Y. Ota, H. Tsunemi, T. Narita, Y. Saito, M. Kohama, M. Suzuki, S. Kishimoto
    IEEE Nuclear Science Symposium Conference Record, 722-726, 2008  Peer-reviewed
    We have been developing a hard X-ray polarimeter with high sensitivity, caBed as a PHENEX (polarimetry for High ENErgy X rays) polarimeter. We constructed prototype PHENEX polarimeter and carried out a preliminary observation of the Crab Nebula on Jun. 13th 2006 as a baUoon-borne experiment. Though we confirmed from the data that PHENEX polarimeter detected hard X rays from the Crab Nebula with a significance of 8σ, the degree and the direction of polarization with high accuracy could not be determined because of the trouble for attitude control system (ACS) and the smaU detection area of the prototype polarimeter. Now we are fixing the ACS trouble and improving the detector to realize the observation of the Crab Nebula with higher accuracy in the next baBoonborne experiment. this paper, we will mainly explain about the improvement of the PHENEX polarimeter and present the expected performance for the next observation. ©2008 IEEE.
  • M. Arimoto, Y. Kanai, M. Ueno, J. Kataoka, N. Kawai, T. Tanaka, K. Yamamoto, H. Takahashi, T. Mizuno, Y. Fukazawa, M. Axelsson, M. Kiss, C. Marini Bettolo, P. Carlson, W. Klamra, M. Pearce, P. Chen, B. Craig, T. Kamae, G. Madejski, J. S.T. Ng, R. Rogers, H. Tajima, T. S. Thurston, Y. Saito, T. Takahashi, S. Gunji, C. I. Bjornsson, S. Larsson, F. Ryde, G. Bogaert, G. Varner
    Physica E: Low-Dimensional Systems and Nanostructures, 40(2) 438-441, Dec, 2007  Peer-reviewed
    Measurements of polarization play a crucial role in the understanding of the dominant emission mechanism of astronomical sources. Polarized Gamma-ray Observer-Light version (PoGOLite) is a balloon-borne astronomical soft gamma-ray polarimeter at the 25-80 keV band. The PoGOLite detector consists of a hexagonal close-packed array of 217 Phoswich detector cells (PDCs) and side anti-coincidence shields (SASs) made of BGO crystals surrounding PDCs. Each PDC consists of a slow hollow scintillator, a fast scintillator and a BGO crystal that connects to a photomultiplier tube at the end. To examine the PoGOLite's capability and estimate the performance, we conducted experiments with the PDC using radioisotope 241Am. In addition, we compared this result with performance expected by Monte Carlo simulation with Geant4. As a result, we found that the actual PDC has the capability to detect a 100 m Crab source until 80 keV. © 2007 Elsevier B.V. All rights reserved.
  • Y. Kishimoto, S. Gunji, Y. Ishigaki, M. Kanno, H. Murayama, C. Ito, F. Tokanai, K. Suzuki, H. Sakurai, T. Mihara, M. Kohama, M. Suzuki, A. Hayato, K. Hayashida, N. Anabuki, M. Morimoto, H. Tsunemi, Y. Saito, T. Yamagami, S. Kishimoto
    IEEE Transactions on Nuclear Science, 54(3) 561-566, Jun, 2007  Peer-reviewed
    We have been developing an instrument named "PHENEX (Polarimetry for High ENErgy X rays)" to measure polarization in the hard X-ray region. The PHENEX polarimeter consists of detector modules called "unit counters". We have investigated the performance of the unit counter, using a highly polarized beam in KEK-PF BL14A. From these measurements, we obtained a detection efficiency of 20% and a modulation factor (analyzing power for polarization) of 53% for 80 keV X rays. Assembling four unit counters, a balloon-flight version was constructed and a preliminary observation of the Crab Nebula was carried out on Jun. 13th, 2006. During this flight, the PHENEX polarimeter observed the Crab for about one hour and detected its hard X rays with a significance of 9ω. From this result, we expect that a PHENEX polarimeter with nine "unit counters" would achieve a 17% minimum detectable polarization of the Crab Nebula with 3ω significance in a 3-hour observation. © 2007 IEEE.
  • 入交芳久, 落合啓, 笠井康子, 山上隆正, 斎藤芳隆, 飯嶋一征, 井筒直樹, 並木道義, 冨川喜弘, 村田功, 佐藤薫
    大気球シンポジウム: 平成18年度, 83-86, Feb, 2007  
  • Y. Kanai, M. Ueno, J. Kataoka, M. Arimoto, N. Kawai, K. Yamamoto, T. Mizuno, Y. Fukazawa, M. Kiss, T. Ylinen, C. Marini Bettolo, P. Carlson, W. Klamra, M. Pearce, P. Chen, B. Craig, T. Kamae, G. Madejski, J. S.T. Ng, R. Rogers, H. Tajima, T. S. Thurston, Y. Saito, T. Takahashi, S. Gunji, C. I. Bjornsson, S. Larsson, F. Ryde, G. Bogaert, S. Kishimoto
    Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 570(1) 61-71, Jan 1, 2007  Peer-reviewed
    We report about the beam test on a prototype of the balloon-based astronomical soft gamma-ray polarimeter, PoGOLite (Polarized Gamma-ray Observer - Light Version) conducted at KEK Photon Factory, a synchrotron radiation facility in Japan. The synchrotron beam was set at 30, 50, and 70 keV and its polarization was monitored by a calibrated polarimeter. The goal of the experiment was to validate the flight design of the polarimeter. PoGOLite is designed to measure polarization by detecting a Compton scattering and the subsequent photo-absorption in an array of 217 well-type phoswich detector cells (PDCs). The test setup included a first flight model PDC and a front-end electronics to select and reconstruct valid Compton scattering events. The experiment has verified that the flight PDC can detect recoil electrons and select valid Compton scattering events down to 30 keV from background. The measure azimuthal modulations (34.4%, 35.8% and 37.2% at 30, 50, and 70 keV, respectively) agreed within 10% (relative) with the predictions by Geant4 implemented with dependence on the initial and final photon polarizations. © 2006 Elsevier B.V. All rights reserved.
  • S. Gunji, H. Sakurai, F. Tokanai, Y. Kishimoto, M. Kanno, Y. Ishikawa, K. Hayashida, N. Anabuki, H. Tsunemi, T. Mihara, M. Kohama, M. Suzuki, Y. Saito, T. Yamagami
    Proceedings of SPIE - The International Society for Optical Engineering, 6686, 2007  Peer-reviewed
    We have been developing a hard X-ray Polarimeter to open a new window for hard X-ray astronomy. The project is called as PHENEX (Polarimetry for High ENErgy X rays). The PHENEX detector is Compton scattering type Polarimeter and it is constructed by several unit counters. The unit counter can achieve the modulation factor and the detection efficiency of 53% and 20% at 80 keV, respectively. Installing four unit counters, we have carried out balloon-borne experiment in Jun. 13 2006 to preliminarily observe the polarization of the Crab Nebula in hard X-ray band. The PHENEX Polarimeter successfully operated on the level flight and observed the Crab Nebula for about one hour. From the analysis of the obtained data, it was recognized that the PHENEX Polarimeter does not make much spurious modulation and that the ratio of the signal from the Crab Nebula to the background from the blank sky is 1:3. Though we can not precisely determine the degree and the direction of the polarization for the Crab Nebula because of the trouble of the attitude control system, the obtained results were not inconsistent with those in the X-ray band. We will carry out balloon-borne experiment again, fixing the trouble of the attitude control system.
  • M. Kanno, S. Gunji, Y. Kishimoto, H. Murayama, Y. Ishigaki, F. Tokanai, H. Sakurai, Y. Ishikawa, K. Katayama, K. Hayashida, M. Morimoto, N. Anabuki, H. Tsunemi, Y. Saito, T. Yamagami, T. Mihara, M. Kohama, M. Suzuki, S. Kishimoto
    2007 IEEE NUCLEAR SCIENCE SYMPOSIUM CONFERENCE RECORD, VOLS 1-11, 399-405, 2007  Peer-reviewed
    We have been developing a hard X-ray polarimeter called "PHENEX" (Polarimetry for High ENErgy X rays). The PHENEX is Compton-scattering-type polarimeter. It is constructed from an array of identical small polarimeter called "unit counter". In Jun. 13 2006, we had carried out balloon-borne experiment to study the polarization of hard X rays from the Crab Nebula, loading the PHENEX polarimeter with four unit counters surrounded by active shields of CsI (TI). The PHENEX accomplished the level flight at the altitude of 37.5 km over 6 hours and the detector system operated well over the duration. However, attitude control system did not function correctly and the line of the sight wandered around the Crab Nebula. Even so the PHENEX polarimeter can observe the Crab Nebula for about one hour and also a blank region of the sky for about one hour. Calculating the effect of the wandering by computer simulation, we carried out the analysis about the polarization of the Crab Nebula. Though the statistical error is large and the significance is low, the modulation to indicate the polarization can be found for the data of Crab Nebula. In near future, we will carry out balloon borne experiment again, improving the PHENEX polarimeter and fixing the trouble of the attitude control system.
  • Kanno Makoto
    Meeting Abstracts of the Physical Society of Japan, 62 102-102, 2007  
  • Meeting Abstracts of the Physical Society of Japan, 62 101-101, 2007  
  • Anabuki Naohisa, Yamada Kazuhiko, Mihara Tatehiro, Sato Tetsuya, Nakajo Hirotaka, Kohama Mitsuhiro, Hayashida Kiyoshi, Ohta Yukihiro, Tsunemi Hiroshi, Gunji Syuichi, Kishimoto Yuji, Ishikawa Yushi, Kanno Makoto, Saito Yoshitaka
    Meeting Abstracts of the Physical Society of Japan, 62 110-110, 2007  
  • Kishimoto Yuji
    Meeting Abstracts of the Physical Society of Japan, 62 111-111, 2007  
  • K. Yoshida, S. Torii, T. Tamura, H. Kitamura, T. Yamagami, J. Chang, I. Iijima, A. Kadokura, K. Kasahara, Y. Katayose, T. Kobayashi, Y. Komori, Y. Matsuzaka, K. Mizutani, H. Murakami, M. Namiki, J. Nishimura, S. Ohta, Y. Saito, M. Shibata, N. Tateyama, H. Yamagishi, T. Yuda
    Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007, 2(OG PART 1) 59-62, 2007  Peer-reviewed
    We have observed cosmic-ray electrons from 10 GeV to 1 TeV with PPB-BETS by a long duration balloon flight using Polar Patrol Balloon (PPB) in Antarctica. The observation was carried out for 13 days at an altitude of 35 km in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillators inserted between lead plates. The geometrical factor of detector is about 600 cm2sr and the total thickness of lead absorber is 9 radiation lengths. We have collected 5.7103 events over 100 GeV including nearly 100 candidates of primary electrons. During the flight, sun aspect sensors and geomagnetic aspect sensors operated to determine the attitude of the instrument. The arrival directions of high-energy electrons over 100 GeV, together with the energy spectrum, are suggested to be a powerful probe to identify nearby cosmic- ray electron sources. In this paper, we present the energy spectrum and arrival directions of cosmic-ray electrons from 100 GeV to 1 TeV observed with PPB-BETS.
  • N. Sakaki, Y. Takizawa, Y. Kawasaki, M. Sato, T. Sawabe, M. Nagano, T. Tsunoda, T. Kamioka, K. Hayasaka, M. Kamimura, A. K. Yoshida, T. Shibata, T. Ebisuzaki, K. Inoue, F. Kajino, Y. Takahashi, Y. Saito, K. Yamada, T. Kawasaki
    Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007, 5(HE PART 2) 965-968, 2007  Peer-reviewed
    Ultra-high energy cosmic rays (UHECRs) above 100 EeV have been observed with several experiments. Their origin and propagation mechanism are still in mystery mainly due to the low statistics. In order to observe UHECRs with sufficient statistics, the JEM-EUSO mission is going on. In the JEMEUSO mission, fluorescence and ̌Cerenkov light from the extensive air showers induced by UHECRs are observed with a telescope attached to the International Space Station. It is important to study the background (BG) intensity in near UV region (300-400nm) seen from the JEM-EUSO telescope. We launched a balloon at Sanriku Balloon Center of JAXA to investigate the nightglow and the clouds on August 29, 2005. The upward and downward nightglow were measured in the eight near UV bands and the cloud images were recorded with an infrared thermography. In this paper, the detail of the experiment and the results will be reported.
  • M. Kanno, S. Gunji, Y. Kishimoto, H. Murayama, Y. Ishigaki, F. Tokanai, H. Sakurai, Y. Ishikawa, K. Katayama, K. Hayashida, M. Morimoto, N. Anabuki, H. Tsunemi, Y. Saito, T. Yamagami, T. Mihara, M. Kohama, M. Suzuki, S. Kishimoto
    IEEE Nuclear Science Symposium Conference Record, 1 399-405, 2007  Peer-reviewed
    We have been developing a hard X-ray Polarimeter called "PHENEX" (Polarimetry for High ENErgy X rays). The PHENEX is Compton-scattering-type Polarimeter. It is constructed from an array of identical small Polarimeter called "unit counter". In Jun. 13 2006, we had carried out balloon-borne experiment to study the polarization of hard X rays from the Crab Nebula, loading the PHENEX Polarimeter with four unit counters surrounded by active shields of CsI (Tl). The PHENEX accomplished the level flight at the altitude of 37.5 km over 6 hours and the detector system operated well over the duration. However, attitude control system did not function correctly and the line of the sight wandered around the Crab Nebula. Even so the PHENEX Polarimeter can observe the Crab Nebula for about one hour and also a blank region of the sky for about one hour. Calculating the effect of the wandering by computer simulation, we carried out the analysis about the polarization of the Crab Nebula. Though the statistical error is large and the significance is low, the modulation to indicate the polarization can be found for the data of Crab Nebula. In near future, we will carry out balloon borne experiment again, improving the PHENEX Polarimeter and fixing the trouble of the attitude control system. © 2007 IEEE.
  • 橋本樹明, 斎藤芳隆, 澤井秀次郎, 坂井真一郎, 坂東信尚, 小林弘明, 藤田和央, 稲富裕光, 吉光徹雄, 石川毅彦, 山川宏
    大気球シンポジウム, 2007/1/16,相模原, 2007, 2007  Peer-reviewed
  • 大気球シンポジウム集録, 2007  
  • INATOMI Yuko, JIMBO Itaru, ISHIKAWA Takehiko, HASHIMOTO Tatsuaki, SAWAI Shujiro, SAITO Yoshitaka, YOSHIMITSU Tetsuo, SAKAI Shin-ichiro, KOBAYASHI Hiroaki, FUJITA Kazuhisa, BANDO Nobutaka, GOTO Masayuki, YAMAKAWA Hiroshi
    JASMA : Journal of the Japan Society of Microgravity Application = 日本マイクログラビティ応用学会誌, 23(4) 280-280, Nov 30, 2006  
  • INATOMI Yuko, ISHIKAWA Takehiko, HASHIMOTO Tatsuaki, SAWAI Shujiro, SAITO Yoshitaka, YOSHIMITSU Tetsuo, SAKAI Shin-ichiro, KOBAYASHI Hiroaki, FUJITA Kazuhisa, BANDO Nobutaka, GOTO Masayuki, JIMBO Itaru, YAMAKAWA Hiroshi
    JASMA, 23(4) 197-203, Nov 30, 2006  
  • Ken Kobayashi, Saku Tsuneta, Tomonori Tamura, Kazuyoshi Kumagai, Yukio Katsukawa, Masahito Kubo, Yasushi Sakamoto, Naoki Kohara, Takamasa Yamagami, Yoshitaka Saito
    ASTROPHYSICAL JOURNAL, 648(2) 1239-1246, Sep, 2006  Peer-reviewed
    We report on the analysis of a thermal flare observed by a newly developed balloon-borne hard X-ray spectrometer. This instrument uses CdTe detectors and can observe the 20 - 120 keV hard X-ray range, with 3.0 keV energy resolution at 60 keV. During the 2002 May 24 flight, it successfully observed a class M1.1 flare. This flare observation shows no detectable flux above 35 keV, and its spectrum is consistent with a superhot thermal source with the temperature varying from 44 to 20MK. Partial observation of the flare by the RHESSI satellite is consistent with this result. The Nobeyama Radio Polarimeters (NORP) observation of this flare shows no detectable polarization. The NORP light curves show impulsive features at 3.75 GHz that can be explained as thermal gyrosynchrotron emission, and this flux is consistent with observed X- ray spectra if a magnetic field of 275 G is assumed. Slower varying features seen in the NORP data are consistent with the lower temperature ("hot'') thermal source of 10 - 15 MK seen in soft X- rays. We conclude that this flare shows no observable signature of nonthermal electrons, and all observed features are consistent with a purely thermal event. This serves as a strong indication that a nonthermal electron beam is not always the dominant energy source of plasma heating in solar flares.
  • Shoji Torii, Tadahisa Tamura, Kenji Yoshida, Hisashi Kitamura, Takamasa Yamagami, Hiroyuki Murakami, Nobuhito Tateyama, Jun Nishimura, Yoshitaka Saito, Shigeo Ohta, Michiyoshi Namiki, Yukihiko Matsuzaka, Issei Iijima, Masaki Ejiri, Hisao Yamagishi, Akira Kadokura, Makio Shibata, Yusaku Katayose, Katsuaki Kasahara, Kohei Mizutani, Tadashi Kobayashi, Yoshiko Komori, Toshinori Yuda, Jin Chang
    Advances in Polar Upper Atmosphere Research, (20) 52-62, Aug, 2006  Peer-reviewed
    We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000 GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600 cm 2sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7 × 10 3 events over 100 GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100 GeV obtained by an electronic counter. © 2006 National Institute of Polar Research.
  • Torii Shoji, Hasebe Nobuyuki, Miyajima Mitsuhiro, Miyachi Takashi, Hareyama Makoto, Okudaira Osamu, Yamashita Naoyuki, Kodaira Satoshi, Nishimura Jun, Makino Fumiyoshi, Yamagami Takamasa, Saito Yoshitaka, Fuke Hideyuki, Takayanagi Masahiro, Ueno Shiro, Tomita Hiroshi, Tamura Tadahisa, Tateyama Nobuhito, Yoshida Kenji, Okuno Shoji, Hibino Kinya, Yuda Toshinori, Shibata Makio, Katayose Yusaku, Kuramata Shiyuuichi, Ichimura Masakatsu, Uchihori Yukio, Kitamura Hisashi, Kasahara Katsuaki, Murakami Hiroyuki, Kobayashi Tadashi, Komori Yoshiko, Mizutani Kouhei, Terasawa Toshio
    (22), Mar, 2006  
    The Twenty-second Space Utilization Symposium (January 17-19, 2006: Science Council of Japan, Roppongi, Tokyo, Japan)We report the activities on the working group "High Energy Cosmic Ray Observation". We have been developing the CALET instrument on-board the Japanese Experiment Module/ Exposed Facility, JEM/EF, of the ISS. We have successfully concluded the mission concept study and the fundamental technical development. By organizing the working group to prepare the mission proposal, we have done much progress on establishing the international team for instrument development, making a written proposal of the project and constructing a proto-type detector for balloon experiments.Physical characteristics: Original contains color illustrationsMeeting sponsors: The Science Council of Japan, The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS)(JAXA)
  • 鳥居祥二, 山上隆正, 田村忠久, 吉田健二, 北村尚, 安楽和明, 山下太郎, 西村純, 斉藤芳隆, 並木道義, 松坂幸彦, 太田茂雄, 門倉昭, 山岸久雄, 江尻全機, 村上博之, 柴田槙雄, 片寄祐作, 笠原克昌, 小林正, 古森良志子, 水谷興平, 湯田利典, 常進
    宇宙航空研究開発機構報告, JAXA RR-05(012) 57-83, Mar, 2006  Peer-reviewed
  • K. Kodama, Y. Nonoyama, T. Kobayashi, K. Satoh, J. S. Song, J. Nishimura, Y. Saito, T. Yamagami, S. Aoki, M. Hara, T. Hara, J. Kirimura, A. Ariga, T. Ban, T. Fukuda, S. Hiramatsu, K. Hoshino, J. Kawada, N. Koike, M. Komatsu, S. Miyamoto, M. Miyanishi, N. Naganawa, M. Nakamura, T. Nakamura, T. Nakano, K. Narita, M. Natsume, K. Niwa, N. Nonaka, B. D. Park, O. Sato, S. Takahashi, T. Toshito, R. Ohmori, Y. Sato, I. Tezuka
    NEXT GENERATION OF SCIENTIFIC BALLOON MISSIONS, 37(11) 2120-2124, 2006  Peer-reviewed
    The Emulsion Cloud Chamber (ECC) has played important role for the cosmic-ray research. The Micro Segment Chamber (MSC) is a new generation detector evolved from the ECC, which has maximized and extended advantages of ECCs as well as overcome difficulties in the analysis of the events that occur inside the detector. The essential parts of MSC and its application to a balloon experiment for cosmic-ray electron observations are described. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR.
  • Y. Saito, I. Iijima, N. Izutsu, T. Kawasaki, Y. Matsuzaka, M. Namiki, M. Toriumi, T. Yamagami, K. Ichimura, T. Kobayashi, K. Matsushima, T. Nakada
    Advances in Space Research, 37(11) 2026-2032, 2006  Peer-reviewed
    Development of a balloon to fly at higher altitudes is one of the most attractive challenges in scientific balloon technologies. After reaching the highest record setting balloon altitude of 53.0 km using the 3.4 μm film in 2002, we tried to make a thinner balloon film. In 2003, we developed a forming die and an air-ring and succeeded in forming a film with a thickness of 3.0 μm and a width of 220 cm. Using this film, we manufactured a balloon with a volume of 5000 m 3 and succeeded in flying the balloon up to an altitude of 46.0 km. We then searched for a good combination of resins to make a thinner and wider film and obtained films with widths of 280 cm, and a thickness of 3.0 μm at first, and then 2.8 μm. In 2004, we performed balloon experiments making a 30,000 m 3 balloon with the 3.0 μm film and a 5000 m 3 balloon with the 2.8 μm film. Both balloons were well manufactured and reached the highest altitudes of 50.7 and 42.6 km, respectively. © 2005 COSPAR.
  • T. Yamagami, I. Iijima, N. Izutsu, T. Kawasaki, Y. Matsuzaka, M. Namiki, Y. Saito, M. Seo, M. Toriumi, S. Tanaka, K. Matsushima
    Advances in Space Research, 37(11) 2033-2037, 2006  Peer-reviewed
    Launching a large balloon in a limited launching field is a long standing problem in Japan. The largest balloon ever launched successfully was 200,000 m 3 in volume. It was launched in 1973. A larger balloon with a volume of 500,000 m 3 was tried later, but it burst during the ascending phase. For launching balloons with a large lift exceeding 500 kg, the conventional static launching method had the most serious problem with possible damage to the polyethylene film of the balloon caused by the holding mechanism. After that, we had developed a new static launching method to launch balloons with a total lift of 1.0 ton. For launching a large balloon with a total lift above 1.5 ton, the new static launching method had a weak point in that if there was an air bubble in the folded part of the balloon, it may puncture the balloon as it is pushed by a spool. To avoid this problem, we developed a semi-dynamic launching method in 1999 using a launcher fixed to the ground leaving a freedom of rotation around the vertical axis. We have launched some balloons using the method and have gradually enriched our experience in using this system. In 2003, we successfully launched a balloon with a volume of 500,000 m 3 by using the method. This balloon was made of polyethylene films with a thickness of 20 μm and it is the largest balloon ever launched in Japan. © 2006.
  • N. Izutsu, I. Iijima, T. Kawasaki, Y. Matsuzaka, M. Namiki, S. Ohta, Y. Saito, M. Toriumi, T. Yamagami, Y. Ebihara, M. Ejiri, A. Kadokura, N. Sato, H. Yamagishi, Y. Katayose, Y. Tomida, M. Fujii, K. Kasahara, H. Murakami, Y. Konno, S. Uchiyama
    Advances in Space Research, 37(11) 2043-2051, 2006  Peer-reviewed
    Polar patrol balloon experiments were carried out at Syowa Station in Antarctica from 2002 to 2004. Two balloons were launched for the purpose of observing phenomena in the polar atmosphere and one was done for the observation of high energy cosmic electrons. We developed a new housekeeping system including communication device using the Iridium satellite network, an auto-level controller driven by a new program for keeping the flight altitude, and a power management system for solar cells combined with secondary batteries. Two balloons for studying phenomena in the Antarctic atmosphere launched on January 13, 2003 made flights for 18 days and 25 days, respectively. All the housekeeping system worked well during the flights as we expected. Based on these experiments, we adjusted parameters for the altitude control system and the power management system. We launched a balloon for the cosmic electron observation on January 4, 2004. It flew 13 days around the Antarctica with the perfect operation of the onboard housekeeping system. We hope that fruitful scientific results will be obtained from these long-duration flights. © 2006 COSPAR.
  • S. Torii, K. Yoshida, T. Tamura, H. Kitamura, T. Yamagami, N. Tateyama, K. Anraku, T. Yamashita, J. Chang, J. Nishimura, Y. Saito, S. Ohta, M. Namiki, Y. Matsuzaka, I. Iijima, H. Yamagishi, A. Kadokura, K. Kasahara, S. Ogawa, M. Fujii, Y. Tasaki, H. Kaiho, M. Shibata, Y. Katayose, T. Inoue, K. Mizutani, Y. Hirai, H. Murakami, T. Kobayashi, Y. Komori, T. Yuda
    Advances in Space Research, 37(11) 2095-2102, 2006  Peer-reviewed
    We have observed cosmic-ray electrons from 10 to 1000 GeV by a long duration balloon flight using Polar Patrol Balloon (PPB) in Antarctica. The observation was carried out for 13 days at an altitude of 35 km in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillators inserted between lead plates. The geometrical factor of detector is about 600 cm 2 sr and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by the CERN-SPS beam test and also investigated by Monte-Carlo simulations. New telemetry system using a commercial satellite of iridium, power supply by solar batteries, and automatic level control using CPU have successfully been developed and operated during the flight. We have collected 5.7 × 10 3 events over 100 GeV including nearly 100 candidates of primary electrons. © 2005 COSPAR.
  • N. Izutsu, I. Iijima, T. Kawasaki, Y. Matsuzaka, M. Namiki, S. O. Ohta, Y. Saito, M. Toriumi, T. Yamagami, Y. Ebihara, M. Ejiri, A. Kadokura, N. Sato, H. Yamagishi, Y. Katayose, Y. Tomida, M. Fujii, K. Kasahara, H. Murakami, Y. Konno, S. Uchiyama
    NEXT GENERATION OF SCIENTIFIC BALLOON MISSIONS, 37(11) 2043-2051, 2006  
    Polar patrol balloon experiments were carried out at Syowa Station in Antarctica from 2002 to 2004. Two balloons were launched for the purpose of observing phenomena in the polar atmosphere and one was done for the observation of high energy cosmic electrons. We developed a new housekeeping system including communication device using the Iridium satellite network, an auto-level controller driven by a new program for keeping the flight altitude, and a power management system for solar cells combined with secondary batteries. Two balloons for studying phenomena in the Antarctic atmosphere launched on January 13, 2003 made flights for 18 days and 25 days, respectively. All the housekeeping system worked well during the flights as we expected. Based on these experiments, we adjusted parameters for the altitude control system and the power management system. We launched a balloon for the cosmic electron observation on January 4, 2004. It flew 13 days around the Antarctica with the perfect operation of the onboard housekeeping system. We hope that fruitful scientific results will be obtained from these long-duration flights. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved.
  • Y. Kishimoto, S. Gunji, Y. Ishigaki, M. Kanno, H. Murayama, C. Ito, F. Tokanai, K. Suzuki, H. Sakurai, T. Mihara, M. Kohama, M. Suzuki, A. Hayato, K. Hayashida, N. Anabuki, M. Morimoto, H. Tsunemi, Y. Saito, T. Yamagami, S. Kishimoto
    2006 IEEE NUCLEAR SCIENCE SYMPOSIUM CONFERENCE RECORD, VOL 1-6, 421-425, 2006  Peer-reviewed
    We have been developing an instrument termed "PHENEX(Polarimetry for High ENErgy X rays)" to measure polarization in the hard X-ray region. The PHENEX polarimeter consists of detector modules called "unit counters". We have investigated the performance of the unit counter, using a highly polarized beam in KEK-PF BL14A. From these measurements, we obtained a detection efficiency of 20% and a modulation factor (analyzing power for polarization) of 53% for 80 keV X rays. Assembling four unit counters, a balloon-flight version was constructed and carried out a preliminary observation of the Crab Nebula in Jun. 13th, 2006. During this flight, the PHENEX polarimeter observed the Crab for about one hour and detected its hard X rays with a significance of 16 sigma. From this result, we project that a PHENEX polarimeter with nine "unit counters" would detect the hard-x-ray polarization of the Crab Nebula with the significance of 3 sigma in a 3-hour observation.
  • E. Miyata, K. Mukai, K. Ikegami, N. Tawa, N. Anabuki, H. Tsunemi, Y. Ogasaka, K. Tamura, A. Furuzawa, R. Shibata, Y. Haba, H. Kunieda, Y. Saito, T. Yamagami, K. Miyaguchi
    Proceedings of SPIE - The International Society for Optical Engineering, 6266 II, 2006  Peer-reviewed
    We report on a new photon-counting detector possessing unprecedented spatial resolution and moderate spectral resolution for 0.5-100 keV X-rays. It consists of an X-ray charge-coupled device (CCD) and a scintillator. The scintillator is directly coupled to the back surface of the X-ray CCD. Low-energy X-rays below 10keV can be directly detected by the CCD. The majority of hard X-rays above 10keV pass through the CCD but can be absorbed by the scintillator, generating visible photons. We employ the needlelike CsI(Tl) in order to prevent the lateral spread of visible photons. We performed the Monte Carlo simulation with DETECT2000 both to maximize the number of visible photons detected by the CCD and to minimize the lateral spread of visible photons on the CCD. We then fabricated the optimized needlelike CsI(Tl) with 300 μm thick and coupled it on the front surface of the back-illuminated (BI) CCD. The high detection efficiency of BI CCDs in the visible band enables us to collect visible photons emitted from the CsI(Tl) efficiently, leading to the moderate spectral resolution of 30% at 59.5 keV combined with the high detection efficiency for hard X-rays. We plan to perform the hard X-ray imaging balloon-borne experiment, SUMIT, in autumn of 2006 at Brazil. We also describe the details about the balloon system of the SD-CCD.
  • Y. Irimajiri, S. Ochiai, Y. Kasai, T. Yamagami, Y. Saito, N. Izutsu, T. Kawasaki, I. Iijima, M. Namiki, I. Murata, K. Sato
    IRMMW-THz 2006 - 31st International Conference on Infrared and Millimeter Waves and 14th International Conference on Terahertz Electronics, 495-495, 2006  Peer-reviewed
    A balloon-borne superconducting submillimeter-wave limb-emission sounder was developed to measure stratospheric molecules. It carries a 300mm-diameter offset parabolic antenna, a 620-650 GHz heterodyne SIS receiver, and an acousto-optical spectrometer. Tsys(DSB) is less than 460 K at 624-639 GHz with a best value of 330 K(11hv/kB). BSMILES was launched from Japan in 2003 and 2004. All systems operated properly and emission line spectra of O3, ClO, HCl, HO2 etc. were measured. After the observations, the gondola splashed on the Pacific Ocean and was retrieved. ©2006 IEEE.
  • Yoshihisa Irimajiri, Takeshi Manabe, Satoshi Ochiai, Harunobu Masuko, Takamasa Yamagami, Yoshitaka Saito, Naoki Izutsu, Tomomi Kawasaki, Michiyoshi Namiki, Isao Murata
    IEEE Geoscience and Remote Sensing Letters, 3(1) 88-92, Jan, 2006  Peer-reviewed
    A balloon-borne superconducting submillimeterwave limb-emission sounder (BSMILES) was developed to observe thermal emission lines from stratospheric minor constituents. BSMILES carries a 300-mm-diameter offset parabolic antenna, a 624-639-GHz superconductor-insulator-superconductor (SIS) receiver, a three-axis fiber-optical gyroscope, and an acousto-optical spectrometer. BSMILES was launched from the Pacific Coast of Japan. All systems operated properly and emission line spectra of stratospheric gases, such as O 3, HCl, HO2, and O3 isotopes were measured. The system noise temperature in double sideband (DSB) during the flight was less than 460 K over the observing bandwidth with a best value of 330 K that is 11 times as large as the quantum limit (11hv/kB). After the observation, the gondola splashed down in the Pacific Ocean and was retrieved. Almost all instruments were waterproofed, and it has been proved that they are reusable. © 2006 IEEE.
  • K. Yoshida, R. Ohmori, T. Kobayashi, Y. Komori, Y. Sato, J. Nishimura
    Physical Review D - Particles, Fields, Gravitation and Cosmology, 74(8), 2006  Peer-reviewed
    We have observed atmospheric gamma rays from 30 GeV to 8 TeV, using emulsion chambers at balloon altitudes, accumulating the largest total exposure in this energy range to date, SΩT∼6.66m2srday. At very high altitudes, with residual overburden only a few gcm-2, atmospheric gamma rays are mainly produced by a single interaction of primary cosmic rays with overlying atmospheric nuclei. Thus, we can use these gamma rays to study the spectrum of primary cosmic rays and their products in the atmosphere. From the observed atmospheric gamma-ray spectrum, we deconvolved the primary cosmic-ray proton spectrum, assuming appropriate hadronic interaction models. Our deconvolved proton spectrum covers the energy range from 200 GeV to 50 TeV, which fills a gap in the currently available primary cosmic-ray proton spectra. We also estimated the atmospheric muon spectrum above 30 GeV at high altitude from our gamma-ray spectrum, almost without reference to the primary cosmic rays, and compared the estimated flux with direct muon observations below 20 GeV. © 2006 The American Physical Society.
  • 岸本 祐二, 小浜 光洋, 林田 清, 森本 真史, 穴吹 直久, 常深 博, 斎藤 芳隆, 山上 隆正, 石垣 保博, 郡司 修一, 門叶 冬樹, 菅野 誠, 伊藤 智加, 村山 裕章, 櫻井 敬久, 三原 建弘
    日本物理学会講演概要集, 61 98-98, 2006  
  • Anabuki Naohisa
    Meeting Abstracts of the Physical Society of Japan, 61 74-74, 2006  
  • Gunji S.
    Meeting Abstracts of the Physical Society of Japan, 61 98-98, 2006  
  • Kanno Makoto
    Meeting Abstracts of the Physical Society of Japan, 61 74-74, 2006  
  • Hayashida Kiyoshi, Murayama Hiroaki, Sakurai Takahisa, Mihara Tatehiro, Kohama Mitsuhiro, Saito Yoshitaka, Yamagami Takamasa, Anabuki Naohisa, Morimoto Masashi, Tsunemi Hiroshi, Gunji Syuichi, Tokanai Fuyuki, Kishimoto Yuji, Ishigaki Yasuhiro, Kanno Makoto
    Meeting Abstracts of the Physical Society of Japan, 61 73-73, 2006  
  • Y. Kishimoto, S. Gunji, Y. Ishigaki, M. Kanno, H. Murayama, C. Ito, F. Tokanai, K. Suzuki, H. Sakurai, T. Mihara, M. Kohama, M. Suzuki, A. Hayato, K. Hayashida, N. Anabuki, M. Morimoto, H. Tsunemi, Y. Saito, T. Yamagami, S. Kishimoto
    IEEE Nuclear Science Symposium Conference Record, 1 421-425, 2006  Peer-reviewed
    We have been developing an instrument termed "PHENEX(Polarimetry for High ENErgy X rays)" to measure polarization in the hard X-ray region. The PHENEX Polarimeter consists of detector modules called "unit counters". We have investigated the performance of the unit counter, using a highly polarized beam in KEK-PF BL14A. From these measurements, we obtained a detection efficiency of 20% and a modulation factor (analyzing power for polarization) of 53% for 80 keV X rays. Assembling four unit counters, a balloon-flight version was constructed and carried out a preliminary observation of the Crab Nebula in Jun. 13th, 2006. During this flight, the PHENEX Polarimeter observed the Crab for about one hour and detected its hard X rays with a significance of 16 σ. From this result, we project that a PHENEX Polarimeter with nine "unit counters" would detect the hard-x-ray polarization of the Crab Nebula with the significance of 3 σ in a 3-hour observation. © 2006 IEEE.
  • 大気球シンポジウム集録, 2006  
  • INATOMI Y., BANDO N., SAWAI S., ISHIKAWA T., SAKAI S., YOSHIMITSU T., SAITO Y., YAMAKAWA H., HASHIMOTO T.
    JASMA : Journal of the Japan Society of Microgravity Application = 日本マイクログラビティ応用学会誌, 22(4) 317-317, Nov 28, 2005  
  • 高橋渉, 内田正美, 江尻全機, 海老原祐輔, 門倉昭, 斎藤芳隆, 佐藤夏雄, 鈴木裕武, 関育子, 中川道夫, 中村智一, 並木道義, 松坂幸彦, 村上浩之, 山内誠, 山本幹生, 山上隆正, 山岸久雄, その他X線WG
    平成16年度大気球シンポジウム集録, 55-58, Mar, 2005  Peer-reviewed
  • Saito Yoshitaka, Iijima Issei, Izutsu Naoki, Kawasaki Tomomi, Matsuzaka Yukihiko, Namiki Michiyoshi, Toriumi Michihiko, Yamagami Takamasa, Ichimura Koji, Kobayashi Tsutomu, MATSUSHIMA Kiyoho, NAKADA Takashi
    JAXA research and development report, 4 13-33, Feb, 2005  Peer-reviewed
  • NISHIO Yasuho, TOHYAMA Fumio, YAMAGISHI Hisao, KADOKURA Akira, SATO Natsuo, YAMAGAMI Takamasa, SAITO Yoshitaka, NAMIKI Michiyoshi, MATSUZAKA Yukihiko
    JAXA research and development report, 4 89-98, Feb, 2005  Peer-reviewed
    The Polar Patrol Balloon (PPB: Polar Patrol Balloon) Project that was planned for the polar geophysical observations was carried out by the 44-th Japanese Antarctic Research Expedition at Syowa Base, Antarctica in January 2003. Fluxgate magnetometer system was loaded on 3 balloons and the geomagnetic field was measured. It is very difficult to detect vector perturbations of the geomagnetic field by balloon because the motion of the sensors during the flight is irregular and complex. We have developed a high resolution fluxgate magnetometer system that is composed with 8-directional sun pulse sensor, 2-axial clinometer and a pulse clock counter.Two PPBs were launched on 13th January 2003. Their flights were apart 150 km from each other and at an altitude of 31.5 km. We were able to get 2 magnetometers data for 11 days and 25 days respectively. As a result, the attitude change of the gondola were detected but small perturbation of magnetic field vector was undetected because of balloons were not rotated due to spin motor trouble. We describe here the new magnetometer system and results of magnetometer data analysis.
  • IRIMAJIRI Yoshihisa, MANABE Takeshi, OCHIAI Satoshi, YAMAGAMI Takamasa, SAITO Yoshitaka, KAWASAKI Tomomi, IZUTSU Naoki, NAMIKI Michiyoshi, SATO Kaoru, MURATA Isao
    JAXA research and development report, 4 69-76, Feb, 2005  Peer-reviewed
    The second flight of BSMILES (Balloon-borne Superconducting Submillimeter-Wave Limb-Emission Sounder) was conducted on September 7, 2004 to observe stratospheric O3, HCl and so on. An offset parabolic antenna with a diameter of 300 mm, a 620 GHz-band SIS (Superconductor-Insulator-Superconductor) mixer cooled by liquid helium, an AOS (Acousto-Optical Spectrometer), and 3-axes fiber-optic gyroscope are carried in BSMILES. The gondola waslifted to an altitude of about 35 km by a balloon of 100,000 m3 in volume. The system operated normally and emission line spectra of O3, HCl etc. were successfully obtained. The experiment concludes that the retrieved system is reusable.
  • IIJIMA Issei, SAITO Yoshitaka, IZUTSU Naoki, KAWASAKI Tomomi, MATSUZAKA Yukihiko, NAMIKI Michiyoshi, OHTA Shigeo, TORIUMI Michihiko, YAMAGAMI Takamasa, EBIHARA Yusuke, EJIRI Masaki, KADOKURA Akira, SATO Natsuo, YAMAGISHI Hisao, KATAYOSE Yusaku, TOMIDA Yuki, FUJII Mori, MURAKAMI Hiroyuki, UCHIYAMA Sadayuki, KONNO Yuji
    JAXA research and development report, 4 35-53, Feb, 2005  Peer-reviewed
    1984年より国立極地研究所,宇宙科学研究本部,関係大学機関らが中心となり,高緯度地域における気球による長時間科学観測の可能性について南極周回気球PPB(Polar Patrol Balloon)実験が検討されてきた.第44次南極地域観測隊夏季オペレーションにおいてはPPB4機が放球された.宇宙物理観測1機(宇宙電子観測,PPB7号機),地球物理観測3機(オーロラとそれに伴う変動観測,PPB8,9,10号機)である.その内のPPB7号機とPPB9号機はコマンドデコーダーの誤作動により切り離しカッターが働き,気球と観測器が切り離されるという事故が発生した.PPB7号機は放球直前に,PPB8号機は高度15kmに達した時点でカッターが働いた.地球物理観測PPB8号機,PPB10号機は昭和基地より無事に放球され,2〜3週間にわたる観測を行うことができた.無傷のまま地上に残ったPPB7号機は日本に持ち帰り,再び同じような事故が発生しないように誤作動の原因調査・改良を行い,第45次夏季南極プロジェクトで再び放球することになった.本稿では第45次PPB実験の改良点,飛翔結果,HKデータ解析結果を述べる.また,放球設備,Heガス注入量,放球作業は第44次PPB実験と同様であり,詳細は既に2004年度大気球研究報告に紹介されているのでここでは割愛した.
  • Izutsu Naoki, Namiki Michiyoshi, Toriumi Michihiko, Matsuzaka Yukihiko, Kawasaki Tomomi, Iijima Issei, Hirayama Shoji, Seo Motoharu, Saito Yoshitaka, Yamagami Takamasa, Matsushima Kiyoho
    JAXA research and development report, 4 P1-11, Feb, 2005  Peer-reviewed
    Launching a large balloon at a limited launching field is a long standing subject in Japan.The volume of the largest balloon ever launched successfully was 200,000 cubic meters. This type of balloon was firstly launched in 1973. A larger balloon with a volume of 500,000 cubic meters was tried to launch in 1980; however it did not succeed because of burst during the ascending phase. For launching a large balloon with a total lift more than 1 ton, the static launching method, we have used for more than 20 years, has several weak points that may result in failure. We developed a semidynamic launching method using a new launcher, which is fixed on the ground and has a freedom of rotation around the vertical axis and an elevation system up to 5 m, as well as a leap-up spooler system for holding a balloon bubble, in 1999. We have launched several balloons using the method. In 2003, a balloon with a volume of 500,000 cubic meters, which was made of polyethylene films of 20 micro meters in thickness, was successfully launched with the semi-dynamic launching method. It is the largest balloon ever launched in Japan.
  • S. Torii, T. Tamura, T. Yamagami, M. Ejiri, H. Kitamura, I. Iijima, A. Kadokura, K. Kasahara, Y. Katayose, T. Kobayashi, Y. Komori, Y. Matsuzaka, K. Mizutani, H. Murakami, M. Namiki, J. Nishimura, S. Ohta, Y. Saito, M. Shibata, N. Tateyama, H. Yamagishi, K. Yoshida, T. Yuda, J. Chang
    29th International Cosmic Ray Conference, ICRC 2005, 3 29-32, 2005  Peer-reviewed
    We had a long duration balloon flight for observing cosmic-ray electrons from 10 GeV to 1000 GeV by the Polar Patrol Balloon (PPB) in Antarctica. The observation was carried out for 13 days at an average altitude of 35 km in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillators inserted between lead plates. The performance of the detector has been confirmed by the beam test at CERN-SPS and also investigated by Monte-Carlo simulations. We have collected 5.7×103 events above 100GeV including nearly 100 candidates of primary electrons. Preliminary result of the electron energy spectrum in 100̃1000 GeV has been obtained.

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 102

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 1
  • Free text column
    昼休みにも熱心に超小型スーパープレッシャー気球の飛翔制御の研究を行っています(ソフトテニスともいう)。いかに気球に上手に網(ネットではなく、ガット)をかぶせるが重要です。

● 指導学生等の数

 6
  • Fiscal Year
    2018年度(FY2018)
  • Fiscal Year
    2019年度(FY2019)
    Master’s program
    1
    Students under Cooperative Graduate School System
    1
  • Fiscal Year
    2020年度(FY2020)
  • Fiscal Year
    2021年度(FY2021)
    Master’s program
    1
    Students under Cooperative Graduate School System
    1
  • Fiscal Year
    2022年度(FY2022)
    Master’s program
    1
    Students under Cooperative Graduate School System
    1
  • Fiscal Year
    2023年度(FY2023)

● 専任大学名

 2
  • Affiliation (university)
    総合研究大学院大学(SOKENDAI)
  • Affiliation (university)
    総合研究大学院大学(SOKENDAI)

● 所属する所内委員会

 2
  • ISAS Committee
    ISAS News Editors
  • ISAS Committee
    Research Information Committee