Sounding Rocket Research and Operation Grp.
  1. 研究者リスト
  2. 阿部 琢美

阿部 琢美

アベ タクミ  (Takumi ABE)

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 太陽系科学研究系 准教授
総合研究大学院大学（総研大） 物理科学研究科 宇宙科学専攻 准教授
J-GLOBAL ID
200901006137313045
researchmap会員ID
1000253786
外部リンク

研究キーワード

 5

研究分野

 1

経歴

 4

学歴

 3

委員歴

 1

受賞

 1

論文

 124
  • Sorai Teraoka, Huixin Liu, Michi Nishioka, Susumu Saito, Toru Takahashi, Atsushi Kumamoto, Yuki Ashihara, Takumi Abe
    EARTH PLANETS AND SPACE 77(1) 2025年2月25日  
    The measurement of virtual height of the sporadic E layer (h'Es) is very sensitive to the type of ionosonde used and the calibration processes. The ionosondes used by the national institute of communication and technology (NICT) has changed several times in the past, resulting in large differences in h'Es before and after the change. We propose a simple method to calibrate h'Es. We used the data of ionosonde observations at four stations, i.e., Wakkanai (45.16 degrees N, 141.75 degrees E), Tokyo (35.71 degrees N, 139.49 degrees E), Yamagawa (31.20 degrees N, 130.62 degrees E), Okinawa (26.68 degrees N, 128.15 degrees E) to calibrate the latest ionosondes VIPIR2, which were installed in May 2017. We carried out the analysis by applying the double-reflection method to the original ionogram images between 2017 and 2021. By developing an automated image detecting algorithm, we were able to process a large amount of data and achieve a calibration with high accuracy. As a result, it was found that the current VIPIR2 data had an offset of 26-28 km.
  • 佐藤毅彦, 山崎敦, 今村剛, 石井信明, 中村正人, 阿部琢美
    日本惑星科学会誌 遊・星・人 33(1) 74-77 2024年3月  
  • Laila Andersson, Takumi Abe, Hassanali Akbari, Edgar Bering, John W. Bonnell, Anders Eriksson, Jean-Pierre Lebreton, Wojciech Miloch, Sylvain Ranvier
    AIAA SCITECH 2024 FORUM 2024年  
    One of the first instruments used to monitor laboratory plasmas was the Langmuir probe (LP). This instrument is still one of the key sensors in laboratory plasma investigations. With the access to space, the first sounding rockets with Langmuir Probes were flown in 1946-1947; followed with Langmuir probes on satellites from the early 1960s and on Pioneer Venus Orbiter and subsequent interplanetary probes starting in the 1970s. This paper summarizes some of the experiences of using Langmuir probes over the last 75-years in space, what issues have been encountered, and how to overcome different known effects unique to space flight measurements. This work was done through a number of workshops attended by a number of instrument team members and supported by the ISSI organisation.
  • Masatoshi Yamauchi, Johan De Keyser, George Parks, Shin ichiro Oyama, Peter Wurz, Takumi Abe, Arnaud Beth, Ioannis A. Daglis, Iannis Dandouras, Malcolm Dunlop, Pierre Henri, Nickolay Ivchenko, Esa Kallio, Harald Kucharek, Yong C.M. Liu, Ingrid Mann, Octav Marghitu, Georgios Nicolaou, Zhaojin Rong, Takeshi Sakanoi, Joachim Saur, Manabu Shimoyama, Satoshi Taguchi, Feng Tian, Takuo Tsuda, Bruce Tsurutani, Drew Turner, Thomas Ulich, Andrew Yau, Ichiro Yoshikawa
    Experimental Astronomy 54(2-3) 521-559 2022年12月  査読有り
    In the White Paper, submitted in response to the European Space Agency (ESA) Voyage 2050 Call, we present the importance of advancing our knowledge of plasma-neutral gas interactions, and of deepening our understanding of the partially ionized environments that are ubiquitous in the upper atmospheres of planets and moons, and elsewhere in space. In future space missions, the above task requires addressing the following fundamental questions: (A) How and by how much do plasma-neutral gas interactions influence the re-distribution of externally provided energy to the composing species? (B) How and by how much do plasma-neutral gas interactions contribute toward the growth of heavy complex molecules and biomolecules? Answering these questions is an absolute prerequisite for addressing the long-standing questions of atmospheric escape, the origin of biomolecules, and their role in the evolution of planets, moons, or comets, under the influence of energy sources in the form of electromagnetic and corpuscular radiation, because low-energy ion-neutral cross-sections in space cannot be reproduced quantitatively in laboratories for conditions of satisfying, particularly, (1) low-temperatures, (2) tenuous or strong gradients or layered media, and (3) in low-gravity plasma. Measurements with a minimum core instrument package (< 15 kg) can be used to perform such investigations in many different conditions and should be included in all deep-space missions. These investigations, if specific ranges of background parameters are considered, can also be pursued for Earth, Mars, and Venus.
  • 阿部琢美, 渡部重十, YAU Andrew, 北村成寿
    プラズマ・核融合学会誌 98(11) 472-476 2022年11月  
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MISC

 55
  • 阿部 琢美
    真空ジャーナル (178) 10-14 2021年10月  
  • 田寺, 慶樹, 阿部, 琢美, 三宅, 亙
    東海大学紀要. 工学部 57(2) 49-53 2018年3月31日  
  • Masato Nakamura, Nobuaki Ishii, Takeshi Imamura, Takehiko Satoh, Takumi Abe, Chikako Hirose, Atsushi Yamazaki, Junichi Nakatsuka, Tsutomu Ichikawa, Tomoaki Toda, Hiroyuki Toyoda, Sumitaka Tachikawa, Yukio Kamata, Makoto Suzuki, Takao M. Sato, Shin Ya Murakami, Yukio Yamamoto, Naomoto Iwagami, Makoto Taguchi, Tesuya Fukuhara, Shigeto Watanabe, Yukihiro Takahashi, Munetaka Ueno, Manabu Yamada, George L. Hashimoto, Naru Hirata, Toru Kouyama, Kazunori Ogohara, Hiroki Ando, Koichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki
    Proceedings of the International Astronautical Congress, IAC 2016年1月1日  
    Copyright © 2016 by the International Astronautical Federation (IAF). All rights reserved. Japan&#039;s Venus Climate Orbiter Akatsuki was proposed to ISAS (Institute of Space and Astronautical Science) in 2001 as an interplanetary mission. We made 5 cameras with narrow-band filters to image Venus at different wavelengths to track the cloud and minor components distribution at different heights to study the Venusian atmospheric dynamics in 3 dimension. It was launched on May 21st, 2010 and reached Venus on December 7th, 2010. With the thrust by the orbital maneuver engine, Akatsuki tried to go into the westward equatorial orbit around Venus with the 30 hours&#039; orbital period, however it failed by the malfunction of the propulsion system. Later the spacecraft has been orbiting the sun for 5 years. On December 7th, 2015 Akatsuki met Venus again after the orbit control and Akatsuki was put into the westward equatorial orbit whose apoapsis is about 0.44 million km and orbital period of 14 days. Its main target is to shed light on the mechanism of the fast atmospheric circulation of Venus. The systematic imaging sequence by Akatsuki is advantageous for detecting meteorological phenomena with various temporal and spatial scales. We have five photometric sensors as mission instruments for imaging, which are 1 m-infrared camera (IR1), 2 m-infrared camera (IR2), ultra-violet imager (UVI), long-wave infrared camera (LIR), and lightning and airglow camera (LAC). These photometers except LIR have changeable filters in the optics to image in certain wavelengths. Akatsuki&#039;s long elliptical orbit around Venus is suitable for obtaining cloud-tracked wind vectors over a wide area continuously from high altitudes. With the observation, the characterizations of the meridional circulation, mid-latitude jets, and various wave activities are anticipated. The technical issues of Venus orbit insertion in 2015 and the scientific new results will be given in this paper.
  • 阿部 琢美
    平成25年度第1次観測ロケットS-310-42号機・S-520-27号機飛翔実験報告書 SES-TD-14-004 181-183 2015年  
  • 阿部琢美
    ISASニュース (378) 2012年  
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書籍等出版物

 2

講演・口頭発表等

 307
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担当経験のある科目(授業)

 1

所属学協会

 3

Works(作品等)

 2

共同研究・競争的資金等の研究課題

 15
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● 指導学生等の数

 2
  • 年度
    2021年度(FY2021)
    修士課程学生数
    4
    受託指導学生数
    4
    技術習得生の数
    1
  • 年度
    2020年度(FY2020)
    修士課程学生数
    3
    受託指導学生数
    3
    技術習得生の数
    2

● 専任大学名

 1
  • 専任大学名
    総合研究大学院大学（SOKENDAI)

● 所属する所内委員会

 3
  • 所内委員会名
    理学委員会
  • 所内委員会名
    観測ロケット専門委員会
  • 所内委員会名
    スペースチェンバー専門委員会
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