研究者業績

斎藤 芳隆

サイトウ ヨシタカ  (Yoshitaka Saito)

基本情報

所属
国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 学際科学研究系 准教授
学位
博士(理学)(東京大学)
理学(修士)(東京大学)

J-GLOBAL ID
200901068528199528
researchmap会員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。 


学歴

 2

論文

 305
  • 笠原 克昌, 望月 永子, 鳥居 祥二, 立山 暢人, 田村 忠久, 吉田 健二, 大内 達美, 西村 純, 山上 隆正, 斉藤 芳隆, 村上 浩之, 小林 正, 古森 良志子, 本多 守弘, 緑川 章一, 湯田 利典
    宇宙科学研究所報告 特集 41(41) 65-72 2001年2月  査読有り
    最近のスーパーカミオカンデの実験で明らかになったニュートリノ振動に関連して,ニュートリノフラックスの絶対値を求めるためのガンマ線強度の高度変化を気球観測により測定している.観測には,一次電子を観測するために開発されたBETS測定器にガンマ線用のトリガーシステムを付加した装置を用いている.2000年度の観測では,これまでよりトリガーシステムを高性能化することにより,信頼度の高いデータが得られている.データ解析により得られた気球高度でのガンマ線フラックスと,核相互作用モデルの異なるシミュレーション計算の比較により,ニュートリノフラックスの計算に必要なモデルの確定を試みている.資料番号: SA0200063000
  • 並木 道義, 松坂 幸彦, 鳥海 道彦, 内田 右武, 平山 昇司, 小松 俊郎, 本田 秀之, 井筒 直樹, 齋藤 芳隆, 太田 茂雄, 山上 隆正, 廣澤 春任, 松本 敏雄, 兒玉 康資, 本間 容博
    宇宙科学研究所報告 特集 41(41) 25-34 2001年2月  査読有り
    宇宙科学研究所三陸大気球観測所では,スタティック放球方式の一種である立て上げ放球方式を用いて,数多くの大気球の放球を成功させてきた.近年,大型気球の需要が高まり,放球方法の改善と放球場の拡張が必要となっていた.1998年に我々は,新しい大型気球放球装置を用いた放球方法であるセミ・ダイナミック放球方式を開発した.この放球方式は,ガス注入後,ローラー車から気球を解放することによって一気に気球を立て上げ,気球が,観測器直上を固定している大型放球装置の直上にきたとき,大型放球装置から観測器を解放する,という手順で放球を行う.徐々に立てあげていた従来の方式と比べて,ローラーで立て上げて行くときに皮膜を傷つける心配がなくなること,放球作業の時間短縮ができることが利点である.1998年(平成10年)に,飛揚場の先端部分を20m延長し,その延長したほぼ中心部に直径 6 mの回転テーブルを備えた大型気球放球装置を製作した.本ランチャーは,回転テーブルに固定されており,放球時の風向きに合わせて旋回する事が出来る.また,ランチャーに備えた昇降装置により,地面から高さ5mまで観測装置を持ち上げることが可能である.これにより,B1000クラスの大型気球の放球が可能となった.1999年9月6日にこの大型気球放球装置を用いて,最初のテスト気球を放球することに成功し,放球方法および装置の有効性が確認された.資料番号: SA0200061000
  • Y Saito, N Kawai, A Rots, T Kamae, S Shibata
    NEW CENTURY OF X-RAY ASTRONOMY 251 404-405 2001年  査読有り
    We performed 82 ksec observation of the millisecond pulsar PSR B1821-24, the brightest in the X-ray band among the species. It shows a double peaked pulse profile, with peak widths of 80 and 170 musec in FWHM, respectively. The sharper peak coincides approximately with one of the two radio peaks as reported before. The shape of the pulse profile does not depend on energy in 2 to 20 keV band and shows no variation during the observation. The energy spectra of the both peaks are represented by a hard power-law with photon index of 1.1 and no apparent difference in the spectra is found.
  • K. Yoshida, S. Torii, N. Tateyama, T. Tamura, T. Ouchi, T. Kashiwagi, K. Hibino, J. Nishimura, T. Yamagami, Y. Saito, H. Murakami, T. Kobayashi, Y. Komori, K. Kasahara, T. Yuda, M. Ohnishi, M. Shibata, F. Makino
    Advances in Space Research 27(4) 681-686 2001年  査読有り
    The CALET (CALorimetric Electron Telescope) instrument is proposed for the observation of TeV electrons at the Japanese Experiment Module Exposure Facility (JEM/EF) on the ISS, which is composed of an imaging calorimeter with scintillating fibers and lead plates, and a total absorption calorimeter with BGO logs. Since TeV electrons could reach only from the nearby sources within a distance less than 1 kpc, we can expect that the energy spectrum has a structural component and the arrival directions show an anisotropy. Therefore, we should be able to localize and identify the nearby cosmic-ray sources by the TeV electron observation. We report the status of development of the CALET instrument, which has a capability to observe electrons up to 10 TeV and a proton rejection power of ~ 10 6 . We expect to observe ~ 10 3 events over 1 TeV during the 3 years observation. By using the excellent imaging capability of the CALET, gamma-rays over the GeV region and the nuclear components up to 10 15 eV might also be observed. © 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
  • Advances in Space Research 27(4) 675-680 2001年  査読有り
  • Advances in Space Research 26(11) 1867-1870 2001年  査読有り
  • Advances in Space Research 26(11) 1823-1826 2001年  査読有り
  • 大気球シンポジウム集録 2001年  
  • S Torii, T Tamura, N Tateyama, K Yoshida, Y Ouchi, T Yamagami, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, J Nishimura
    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 452(1-2) 81-93 2000年9月  査読有り
    We describe a new detector system developed for high-altitude balloon flights to observe the cosmic-ray electrons above 10 GeV, The Balloon borne Electron Telescope with Scintillating (BETS) fibers instrument is an imaging calorimeter which is capable of selecting electrons against the large background of protons. The calorimeter is composed of a sandwich of scintillating optical-fiber belts and lead plates with a combination of three plastic scintillators for shower trigger. The total thickness of lead is 40 mm ( similar to 7.1 r.l.) and the number of fiber belts is nine. In each belt, alternating layers are oriented in orthogonal (x and y) directions. Two sets of an intensified CCD camera are adopted for read-out of the scintillating fibers in the x and y direction, respectively. The accelerator beam tests were carried out to study the performance of detector for electrons in 1996 and for protons in 1997 at CERN-SPS. The instrument was successfully flown aboard high-altitude balloon in 1997 and 1998. It is demonstrated by the flight data that a reliable identification of the electron component has been achieved in 10-100 GeV and the energy spectrum has been obtained. (C) 2000 Elsevier Science B.V. All rights reserved.
  • T Furusho, NY Yamasaki, T Ohashi, Y Saito, W Voges
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 52(4) 677-684 2000年8月  査読有り
    An ASCA observation of a region containing a Class 0 protostar IRAS 20386 + 6751 in the Lynds 1157 dark cloud, has been carried out. The protostar was not detected, and the 95% upper limit to the luminosity depends on the assumed N-H: L-X(0.5-10 keV) < 1.1 x 10(31) erg s(-1) for N-H = 1 x 10(23) cm(-2). A Class I protostar in Lynds 1152, IRAS 20353 + 6742, in the same field was also undetected with an upper limit about three-times as much as the Lynds 1157 level. Besides these non detections, nine new X-ray sources were detected and a spectral analysis was performed for 4 sources. One object (AX J2038 + 6801) shows a hard spectrum with a temperature of kT similar to 8 keV or a power-law photon index of similar to 2.0 and absorbed with N-H similar to 2 x 10(22) cm(-2). Another fainter one (AX J2036 + 6800) has a soft spectrum with most of the emission falling below 2 keV. We examine the possible nature of these new X-ray sources based on their spectral properties.
  • 鳥居 祥二, 山上 隆正, 村上 浩之, 田村 忠久, 吉田 健二, 立山 暢人, 大内 達美, 斎藤 芳隆, 小林 正, 古森 良志子, 笠原 克昌, 湯田 利典, 西村 純
    宇宙科学研究所報告 特集 40(40) 77-83 2000年3月  査読有り
    BETS (Balloon Borne Electron Telescope with Scintillating Fibers)による, 10GeVから100GeVまでの電子エネルギースペクトルの最新の観測結果を報告する。この装置は, 約10,000本のシンチレーティング・ファイバーと4cm(7.1r.l.)厚の鉛板から構成されたイメージング・カロリメータである。電子選別のために, 陽子の除去を宇宙線シャワーのイメージングによって行っており, その除去能力は約2,500倍であることが確かめられている。この報告では, 1997年と1998年に三陸で行った気球観測の結果について, これまでの他の観測値と比較する。そして, 銀河中での電子の拡散係数やsolar modulationの効果について議論している。資料番号: SA0167159000
  • 斎藤 芳隆, 太田 茂雄, 鳥海 道彦, 並木 道義, 松坂 幸彦, 山上 隆正, 横田 力男, 市村 晃司, 小林 勉, 野沢 聡, 松島 清穂
    宇宙科学研究所報告 特集 40(40) 1-17 2000年3月  査読有り
    宇宙科学研究所気球工学部門では, 10kg程度の観測器をより高高度に到達させる気球を開発している。今回, メタロセンを触媒としたポリエチレンフィルムが気球用フィルムとして適していることを見い出し, これを用いて従来の半分近い厚みである3.4μm厚のフィルムを製作することに成功した。さらに, このフィルムはフィルム自体の強度で熱接着ができることを確認した。また, 熱接着部に入れる補強テープの重量も1/4程度に削減することに成功した。このフィルムとテープを用いて体積1,000m^3の気球を製作し, 1999年9月1日に飛翔性能試験を行った。気球は正常に上昇し, 最大到達高度37kmに到達した。この実験は, 大型の超薄型プラスチック気球開発の目処をつけたという点で非常に画期的なものであった。資料番号: SA0167153000
  • Y Matsuzaka, T Yamagami, M Namiki, M Toriumi, S Ohta, F Makino, H Hirosawa
    SCIENTIFIC BALLOONING 26(9) 1365-1368 2000年  査読有り
    The development of high altitude balloons will enrich many areas of scientific observation. A high altitude balloon fabricated using improved technology with thin Winzen polyethylene films has been flown in the upper atmosphere. A light weight balloon carrying small instruments can reach an altitude higher than 40 km. In contrast to sounding rockets, the balloon-borne experiment provides a unique opportunity to stay at a high altitude for more than a few hours at low cost. We have developed methods for fabricating large balloons for scientific observation and have also established a new belt sealer and successful launching system. In January 27, 1997, a thin-film balloon with a volume of 120,000 m(3), carrying a payload of 11.8 kg, reached an altitude of 50.2 km which is the highest balloon altitude ever in Japan. This shows that a thin-film balloon is suitable for high altitude observations and can fill the gap between satellite and conventional balloon altitudes. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  • Advances in Space Research 26(9) 1353-1356 2000年  査読有り
  • Saito Yoshitaka, Matsuzaka Yukihiko, Miyahara Yasuaki, Ohnishi Akira, Yamagami Takamasa, Yokota Rikio, Kobayashi Tadashi, Nishimura Jun
    Advances in polar upper atmosphere research 14 163-171 2000年  査読有り
    Large plastic balloon play an important role for scientific observations at high altitude in the field of astrophysics and geophysics. In these observations, it has been well recognized that the long duration balloon flights are indispensable for precise observations. For a normal zero pressure balloon, we need to drop ballast to keep a level altitude during day and night to prevent from altitude excursions. This is due to the temperature change of lifting gas, and the duration of the balloon is limited when all the ballast on board the balloon has been exhausted. In this paper, we discuss a possibility of minimizing the temperature variation of the lifting gas using specific balloon films with suitable optical properties and show the optical properties of some test films for this purpose.
  • S Torii, N Tateyama, T Tamura, T Ouchi, K Kashiwagi, K Yoshida, K Hibino, Y Yamagami, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, M Ohnishi, M Shibata, F Makino, J Nishimura
    SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM, PTS 1 AND 2 504 187-192 2000年  
    The CALET instrument is proposed for the Japanese Experiment Module/ Exposure Facility (JEM/EF) on International Space Station (ISS) to resolve the long-term puzzles in high-energy cosmic-ray physics. The ISS gives us a unique opportunity to carry out the measurements of cosmic ray electrons with a relatively heavy and large detector, and for the long exposure. The instrument will be composed of an imaging calorimeter with scintillating fibers and a total absorption calorimeter for detecting the electrons up to 10,000 GeV. The origin of high-energy electrons and the diffusion characteristics in the Galaxy will be revealed by measuring the energy spectrum of electrons and the anisotropy of arrival directions. By the excellent capability of the CALET, both of the gamma-rays over GeV and nucleus component up to 10(15)eV might be investigated as additional possibilities of the observation.
  • M Takahashi, S Shibata, K Torii, Y Saito, N Kawai, M Hirayama, T Dotani, S Gunji, H Sakurai
    PULSAR ASTRONOMY - 2000 AND BEYOND: IAU COLLOQUIUM 177 202 353-354 2000年  
    We report the first detection of the pulsed X-ray emission from the fastest millisecond pulsar known PSR B1937+21 (P =1.558msec) with ASCA. The pulsar is detected as a point source above similar to 1.7keV, with no nebulosity indicated. The source flux in the energy band 2-10keV is found to be f = 4.3 x 10(-13)erg s(-1) cm(-2), which corresponds to the luminosity of L-x = 4 pi D(2)f approximate to 6.6 x 10(32)(D/3.6kpc)(2) erg s(-1), where D is the distance, and correspond to approximate to 6 x 10(-4) of the rotation power of the pulsar. The pulsation is found at the period predicted by the radio ephemerides with very narrow primary peaks, the width of which is about 1/16 phase approximate to 100 mu s near the time resolution limit (61 mu s) of the observation. The pulsed luminosity within the primary peak (1/16 phase interval) is found to be f(p) = 4.0 x 10(-12)erg s(-1) cm(-2) Although there may be a secondary peak, its statistical significance is too low to identify. Spectra of the whole source region and the primary peak are fitted by power law models to give photon indices of about unity for both.
  • T Oka, N Kawai, T Naito, T Horiuchi, M Namiki, Y Saito, RW Romani, T Kifune
    ASTROPHYSICAL JOURNAL 526(2) 764-771 1999年12月  査読有り
    CO J = 1-0 mapping observations of the dark nebula Lynds 227, which is possibly associated with the unidentified EGRET source 2EG J1811-2339, are presented. We detected a large amount of molecular gas along Lynds 227 with a total mass of (1-2) x 10(4) M-circle dot surrounding an X-ray synchrotron nebula, which was detected by the ASCA within the error circle of 2EG J1811-2339. Molecular gas along Lynds 227 shows spatial anticorrelation with the X-ray synchrotron nebula, suggesting that the synchrotron nebula is interacting with the Lynds 227 cloud. We propose a gamma-ray emission mechanism for 2EG J1811-2339: high-energy electrons are injected from a rotation-powered pulsar and further accelerated in shock waves generated by the interaction with ambient matter. The high-energy electrons move into the molecular cloud at the Lynds 227 and collide with dense interstellar matter to yield high-energy gamma-ray photons, mainly through relativistic bremsstrahlung.
  • K Torii, H Tsunemi, T Dotani, K Mitsuda, N Kawai, K Kinugasa, Y Saito, S Shibata
    ASTROPHYSICAL JOURNAL 523(1) L69-L72 1999年9月  査読有り
    We report here the first measurement of the spin-down rate of the 65 ms X-ray pulsar within the supernova remnant G11.2-0.3. The period derivative is measured to be (P)over dot = (4.40(-0.04)(+0.03)) x 10(-14) s s(-1) using the Advanced Satellite for Cosmology and Astrophysics and BeppoSAX. From the pulsar period and its derivative, the corresponding surface magnetic field (B = 1.7 +/- 10(12) G) and the characteristic age [P/(2(P)over dot) = 2.4 x 10(4) yr] are derived. The physical association of the pulsar and supernova remnant with the historical record of A.D. 386 is discussed in the context of the measured (P)over dot. If the pulsar was formed during the historical event, the initial pulse period should have been relatively slow (P-0 similar or equal to 62 ms). This initial period is more than a factor of 3 larger than that of a small number of prototypical objects, suggesting a diversity of initial periods for newly formed neutron stars.
  • Sakurai, I, N Kawai, H Negoro, K Torii, Y Saito, S Shibata
    ASTRONOMISCHE NACHRICHTEN 320(4-5) 339-339 1999年  査読有り
    We report results for the X-ray spectrum of a millisecond pulsar, PSR J2124-3358 observed with ASCA. This pulsar is an isolated 4.9 ms pulsar (Bailes et al 1997). Its X-ray pulsation was detected with ROSAT HRI in the 0.1- 2.4 keV band(Becker & Trumper 1998). The pulse profile was broad, and there is an indication of a secondary peak. Due to the lack of spectral information, the nature of the S-ray emission was unclear. An ASCA observation of this pulsar was carried out in May 1998, and provided the X-ray spectrum in the energy band from 0.5 to 10.0 keV. Due to poor statistics, the X-ray pulsation was not confirmed by ASCA.
  • K Torii, H Tsunemi, T Dotani, K Mitsuda, N Kawai, K Kinugasa, Y Saito, S Shibata
    ASTRONOMISCHE NACHRICHTEN 320(4-5) 343-343 1999年  査読有り
  • M Takahashi, S Shibata, S Gunji, H Sakurai, K Torii, Y Saito, N Kawai, T Dotani, M Hirayama
    ASTRONOMISCHE NACHRICHTEN 320(4-5) 340-340 1999年  査読有り
  • N Kawai, Y Saito
    ASTROPHYSICAL LETTERS & COMMUNICATIONS 38(1-6) 1-8 1999年  査読有り
    The non-thermal magnetospheric X-ray emission from rotation-powered pulsars can be studied best in the energy band above 2 keV where the contamination by the thermal component is less significant than in the soft X-ray band. With the recent advances in the high sensitivity X-ray observations, X-ray pulsations are found from more pulsars including several millisecond pulsars. We review the recent progress in the X-ray observations of the millisecond pulsars, and show that the emission properties have strong correlation with the magnetic field strength at the light cylinder.
  • S Torii, N Tateyama, T Tamura, T Ouchi, K Kashiwagi, K Yoshida, K Hibino, T Yamagami, Y Saito, H Murakmai, T Kobayashi, Y Komori, K Kasahara, T Yuda, M Ohnishi, M Shibata, J Nishimura
    SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - 1999, PTS ONE AND TWO 458 127-132 1999年  査読有り
    By using the JEM (Japanese Experiment Module) facility on ISS, we are planning to carry out a precise measurement of the flux and energy spectrum of cosmic-ray electrons of 10 GeV to several TeV. Since the electrons over several 100 GeV could be contributed only from the nearby sources within a distance less than 1 kpc, it is expected in the high energy region that the energy spectrum has a structural component and the distribution of the arrival directions presents anisotropy. By helping to localize and identify the nearest cosmic ray sources, these data should help to resolve the long-term puzzle. The instrument used for the observation is a kind of scintilating-fiber/lead imaging calorimeter that has been used for the balloon observations. We are developing an improved detector having a geometrical factor of 0.5 m(2)sr and a higher rejection power against the background protons ( greater than or equal to 10(4)). It is expected to observe nearly 500 electrons over 1 TeV during the one-year observation.
  • Oka T, Kawai N, Naito T, Horiuchi T, Namiki M, Saito Y, Romani R. W, Kifune T
    Astronomische Nachrichten 320(4-5) 327 1999年  
  • Kokubun M, Fukazawa Y, Idesawa E, Kataoka J, Kamae T, Matsuzaki K, Mizuno T, Saito Y, Takahashi T, Takizawa K, Tashiro M, Tamura T, Yoshida A
    IEEE Nuclear Science Symposium and Medical Imaging Conference 1 227-232 1999年  査読有り
  • 大気球シンポジウム集録 73 1999年  
  • 中性子星の誕生と進化研究会集録 127 1999年  
  • 超高エネルギー天体研究会集録 85 1999年  
  • M. Kokubun, Y. Fukazawa, E. Idesawa, J. Kataoka, T. Kamae, K. Matsuzaki, T. Mizuno, Y. Saito, T. Takahashi, K. Takizawa, M. Tashiro, T. Tamura, A. Yoshida
    IEEE Transactions on Nuclear Science 46(3) 371-376 1999年  
    ASTRO-E Hard X-ray Detector (HXD) is characterized by well-type phoswich counters[1] in a compound-eye configuration which reduce the detector background to lower level than any other past hard X-ray mission. When operating in Low Earth Orbit, the expected background of the HXD is an order of 10 -5 counts/s/kcV/cm 2, mainly caused from the radioactivity induced within the detector materials by geomagnetically trapped protons. Results are presented from measurements of induced radioactivity in two phoswich scintillators, GSO (Gd 2SiO 5:Ce 0.5% mol) and BGO (Bi 4Ge 3O 12), irradiated by mono-energetic protons at an accelerator facility. Radiation transport computer codes are used to build the detector response functions for emissions from decays of spallation products. Based on the comparison between experimental and simulation results, the activation background level of HXD in the orbit is estimated. © 1999 IEEE.
  • Y Saito, E Mochizuki, T Yamagami, N Kawai
    ASTRONOMISCHE NACHRICHTEN 320(4-5) 329-329 1999年  
  • Saito Yoshitaka, Yamagami Takamasa, Nishimura Jun
    Advances in polar upper atmosphere research 13 182-190 1999年  査読有り筆頭著者
    For long duration balloon flights, when the balloon is outside the tele-command range, it is necessary to control the altitude automatically since the temperature of the lifting gas decreases at sunset. Here, we propose a new method referring to the inner pressure at the nadir of a balloon. The inner pressure is approximately proportional to the amount of descent from the level altitude and to the atmospheric pressure at the level altitude. This method has advantages in its simplic- ity and does not require prior information of the level altitude.
  • AH Rots, K Jahoda, DJ Macomb, N Kawai, Y Saito, VM Kaspi, AG Lyne, RN Manchester, DC Backer, AL Somer, D Marsden, RE Rothschild
    ASTROPHYSICAL JOURNAL 501(2) 749-757 1998年7月  査読有り
    Observations with the Rossi X-Ray Timing Explorer and the Jodrell Bank, Parkes, and Green Bank telescopes have enabled us to determine the time delay between radio and X-ray pulses in the two isolated pulsars B1821-24 and B1509-58. For the former we find that the narrow X-ray and radio pulse components are close to being coincident in time, with the radio peak leading by 0.02 period (60 +/- 20 mu s), while the wide X-ray pulse component lags the last of the two wider radio components by about 0.08 period. For the latter pulsar we find, using the standard value for the dispersion measure, that the X-ray pulse lags the radio by about 0.27 period, with no evidence for any energy dependence in the range 2-100 keV. However, uncertainties in the history of the dispersion measure for this pulsar make a comparison to previous results difficult. It is clear that there are no perceptible variations in either the lag or the dispersion measure at timescales of a year or less.
  • JP Finley, R Srinivasan, Y Saito, M Hiriyama, T Kamae, K Yoshida
    ASTROPHYSICAL JOURNAL 493(2) 884-890 1998年2月  査読有り
    The young "Vela"-like neutron star PSR B1706-44 was imaged by both the HRI aboard ROSAT and the solid-state imaging spectrometers and gas imaging spectrometers aboard ASCA during a 6 month period in late 1994 and early 1995. The broadband data set, extending over two decades in energy, allowed a detailed spatial, spectral, and temporal study to be conducted. PSR B1706-44 is found embedded in a compact synchrotron nebula of physical size similar to 0.32 pc and displays the morphology characteristic of the other young neutron stars in the 10(4)-10(5) yr age range. No pulsations at the radio period were detected in either the ROSAT or the ASCA data. The spectrum is well described by a power-law distribution, and the data are consistent with there being no spectral break from the radio through the soft X-ray band. The unpulsed TeV emission that has been observed from PSR B1706-44 can be reconciled with these observations if the TeV emission results from the up-scattering of background IR photons by the population of high-energy particles that produce the soft X-ray photons.
  • N Kawai, K Tamura, Y Saito
    SPACE BASED ASTRONOMY: ISO, AGN, RADIOPULSARS AND THE SUN 21(1-2) 213-221 1998年  査読有り
    Results from the X-ray observations of pulsars with ASCA are presented. The surroundings of pulsars are investigated in detail taking advantage of ASCA's unique capabilities; high spectral resolution and a high throughput over a wide energy range from 0.4 keV to 10 keV. We detected diffuse emission sources in the vicinity of many pulsars, often with asymmetric structure. The high probability of finding such diffuse sources for many pulsars suggests that they exist universally for all the active pulsars, and that they are powered by the pulsars. The results of the ASCA observation of the two millisecond pulsars, PSR J0437-4715 and PSR B1821-24 are presented. They have very different characteristics. The energy spectrum of PSR J0437-4715 is best described by a blackbody with kT=0.27 keV. PSR B1821-24, on the contrary, has a hard X-ray spectra. A non-thermal sharp pulsed emission was detected. (C) 1998 COSPAR. Published by Elsevier Science Ltd.
  • 斎藤芳隆
    原子核研究 42(6) 1998年  
  • 大気球シンポジウム集録 68 1998年  
  • R Danner, Kulkarni, SR, Y Saito, N Kawai
    NATURE 388(6644) 751-753 1997年8月  
    Globular clusters, the most ancient stellar groups in our galaxy, are known to contain bright X-ray sources, faint X-ray sources and millisecond pulsars, The bright X-ray sources are neutron stars accreting matter from a companion star(1), and the millisecond pulsars are believed to be descendants of these sources(2). But the origin of the faint X-ray sources remains unclear Here we report satellite-based X-ray observations of the globular cluster M28 which reveal two faint X-ray sources; an extended source slightly offset from the centre of the duster, and a point source. The point source pulsates with the same period as a well-known(3,4) 3-millisecond pulsar in M28. The nature of the extended source is more puzzling, however, and its spatial and spectral properties permit a range of plausible models. We argue that this source is either a collection of low-luminosity accreting neutron-star binaries or a synchrotron nebula powered by a recent outburst of energy from an unknown source. Sensitive optical and X-ray observations should be able to distinguish between these two possibilities.
  • Y Saito, N Kawai, T Kamae, S Shibata, T Dotani, Kulkarni, SR
    ASTROPHYSICAL JOURNAL 477(1) L37-L40 1997年3月  査読有り筆頭著者
    We report the first clear detection of X-ray pulsation of magnetospheric origin from a millisecond pulsar, PSR B1821-24, with the Advanced Satellite for Cosmology and Astrophysics. The photon arrival time shows a periodicity of 3.05 ms period, as observed in the radio band. The observed X-ray pulse is double peaked. The pulses are characterized by a sharp temporal profile and hard power-law spectrum with a phase-averaged photon index of similar to 1.9. These two features are quite similar to the X-ray/y-ray pulses from the Crab pulsar and characteristic of the nonthermal emission from the magnetosphere of the neutron star, but contradictory to the thermal emission from its surface. Since this pulsar has physical parameters completely different from those of young pulsars, we expect these observations to provide significant constraints on models of pulsar magnetospheric emission, which have been developed mostly based on the observations of young pulsars.
  • 大気球シンポジウム集録 1997年  
  • Y Saito, N Kawai, T Kamae, S Shibata
    PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2 (410) 628-632 1997年  
    We observed 8 pulsars with high spin down flux and searched for pulsation in the X-ray band (0.6-10 keV) with ASCA. We detected X-ray emission from all pulsars, including new detection in the 2-10 keV band for 3 pulsars. We also found pulsed emission from 3 pulsars including the first detection of millisecond pulsar PSR B1821-24 [1]. The pulse of PSR B1821-24 has sharp double peaks similar to that of the Crab pulsar and power-law spectrum which strongly suggest the magnetospheric origin. We found an empirical relation between the pulsed luminosity L-X(pulse) and the rotation energy loss (E) over dot(rot) in the X-ray band among all X-ray pulsars observed with ASCA. The pulsed luminosity is consistent with the relation L-X(pulse) proportional to (E) over dot (3/2)(rot), while those Tor the pulsed emission in gamma-ray band L-gamma(pulse) is L-gamma(pulse) proportional to (E) over dot(rot)(1/2). It should he noted that the empirical relation in the X-ray band holds also for the millisecond pulsar PSR B1821-24, which suggests same pulse emission mechanism works for millisecond pulsars.
  • T Takahashi, H Ezawa, Y Fukazawa, M Hirayama, E Idesawa, H Ikeda, Y Ishisaki, N Iyomoto, T Kamae, J Kataoka, H Kaneda, H Kubo, K Makishima, K Matsushita, K Matsuzaki, T Mizuno, T Murakami, K Nagata, S Nakamae, M Nomachi, H Obayashi, T Ohtsuka, H Ozawa, Y Saito, M Sugizaki, T Tamura, M Tashiro, N Tsuchida, K Tsukada, A Yoshida
    ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES 120(4) C645-C648 1996年12月  査読有り
    The Hard X-ray Detector (HXD) is one of three instruments on the fifth Japanese X-ray astronomy satellite, ASTRO-E, scheduled for launch in 2000. The HXD consists of a 4x4 = 16 modular assembly of identical counters, each consisting of a combination of YAP(or GSO)/BGO well-type phoswich counters and silicon PIN diodes. The field of view of the detector for high energy photons is restricted to 4 degrees x 4 degrees by active collimators made of BGO and the fov for low energy photons is restricted to 0.5 degrees x 0.5 degrees by the fine passive collimators made of phosphor bronze. The detector is characterized by a low background reaching severalx10(-6) c/s/cm(2)/keV. Combined with the other two instruments for soft X-ray observations (0.5-12 keV), the ASTRO-E mission will cover the entire range of soft and hard X-rays with the highest sensitivity ever achieved. Furthermore, thick EGO counters which surround the 4x4 matrix of well-type phoswich counters act as a gamma-ray burst detector in the energy band of 100-2000 keV.
  • H Ezawa, M Hirayama, T Kamae, H Kubo, K Matsuzaki, K Nagata, Y Saito, H Ikeda, K Tsukada, Y Sano, K Shimizu, H Ozawa, T Takahashi, H Murakami
    1995 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE RECORD, VOLS 1-3 224-228 1996年  査読有り
  • RIKEN Super Computing Prog. Rep. 2 1 1996年  
  • Procs. of X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas 403 1996年  
  • Procs. of X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas 503 1996年  
  • H KANEDA, M TASHIRO, Y IKEBE, Y ISHISAKI, H KUBO, K MAKISHIMA, T OHASHI, Y SAITO, H TABARA, T TAKAHASHI
    ASTROPHYSICAL JOURNAL 453(1) L13-L16 1995年11月  査読有り
    Extended X-ray emission was detected with ASCA from the synchrotron double lobes of the radio galaxy Fornax A. This is thought to be the same emission as was detected with ROSAT. The excess X-rays exhibit very hard spectra, described by a power law of energy index 1.2 +/- 0.5. Since this index is consistent with the synchrotron. radio index of 0.9 +/- 0.2, the X-rays are thought to arise when the radio-emitting relativistic electrons make inverse-Compton scattering off the cosmic microwave photons. Comparison of the X-ray and radio fluxes yields the lobe magnetic field intensity of 2-4 mu G. The relativistic electrons in the lobes are inferred to have an energy density close to that of the magnetic fields.
  • Hidehiro Kaneda, Hajime Ezawa, Masaharu Hirayama, Tuneyoshi Kamae, Hidetoshi Kubo, Keiichi Matsuzaki, Kazuo Makishima, Takanori Ohtsuka, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura, Makoto Tashiro, Naohiko Tsuchida, Toshio Murakami, Mutsumi Sugizaki, Hirokazu Ikeda, Kiwamu Tsukada, Masaharu Nomachi, Shuichi Gunji, Satoshi Miyazaki, Tadahisa Tamura, Noriko Y. Yamasaki, Atsumasa Yoshida
    EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy VI 2518 85-95 1995年9月1日  
    The ASTRO-E satellite is scheduled for launch in 2000 by the Institute of Space and Astronautical Science (ISAS). In this paper the design and performance of the hard x ray detector (HXD) developed for ASTRO-E are described. The HXD is a combination of YAP/BGO phoswich scintillators and silicon PIN diodes covering a wide energy band of 10 - 700 keV. The detector background is reduced down to several times 10 -6c/s/cm 2/keV, and the sensitivity of the HXD is more than one order of magnitude higher than any other past missions in the range of a few 10 keV to several 100 keV. Thus ASTRO-E HXD is expected to achieve an extreme high performance for detecting cosmic hard x rays and low-energy gamma rays. Astrophysics to be explored with the HXT are expected to be extremely widespread and rich.
  • 斎藤 芳隆, 江澤 元, 釜江 常好, 窪 秀利, 鈴木 清詞, 関本 裕太郎, 高橋 忠幸, 田中 光明, 平山 昌治, 松崎 恵一, 矢島 信之, 山上 隆正, 秋山 弘光, 郡司 修一, 田村 忠久, 能町 正治, 宮崎 聡, 村上 浩之, 森 国城, 山崎 典子, EDBERG Tim
    宇宙科学研究所報告. 特集: 大気球研究報告 32(32) 71-88 1995年3月  査読有り
    硬X線/γ線検出器Welcome-1 (mk2)の気球実験における方位角制御のために, リアクションホイールとよじれ戻しモーターを用いた制御方法による方位角制御システムを構築した。制御に用いた部品のパラメーターの評価, 地上, および上空でのパフォーマンスについて報告する。資料番号: SA0167057000
  • M TASHIRO, K MAKISHIMA, H EZAWA, Y FUKAWA, E IDESAWA, Y ISHISAKI, N IYOMOTO, T KAMAE, H KANEDA, K MATSUSHITA, K MATSUZAKI, Y SAITO, Y SEKIMOTO, T TAMURA, M HIRAYAMA, M ISHIDA, H KUBO, K OKADA, T TAKAHASHI, Y UEDA, K KIKUCHI, T OHASHI, NY YAMASAKI, Y KOHMURA, Y IKEBE, T MIHARA, T TSURU, K EBISAWA, S GUNJI
    EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VI 2518 2-12 1995年  査読有り

主要なMISC

 68

主要な講演・口頭発表等

 102

主要な共同研究・競争的資金等の研究課題

 16

● 自由記述

 1
  • ひとこと    
    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
  • 年度
    2018年度(FY2018)
  • 年度
    2019年度(FY2019)
    修士課程学生数
    1
    連携大学院制度による学生数
    1
  • 年度
    2020年度(FY2020)
  • 年度
    2021年度(FY2021)
    修士課程学生数
    1
    連携大学院制度による学生数
    1
  • 年度
    2022年度(FY2022)
    修士課程学生数
    1
    連携大学院制度による学生数
    1
  • 年度
    2023年度(FY2023)

● 専任大学名

 2
  • 専任大学名
    総合研究大学院大学(SOKENDAI)
  • 専任大学名
    総合研究大学院大学(SOKENDAI)

● 所属する所内委員会

 2
  • 所内委員会名
    ISASニュース編集委員会
  • 所内委員会名
    研究情報委員会