深宇宙追跡技術グループ

戸田 知朗

トダ トモアキ  (Tomoaki Toda)

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 宇宙機応用工学研究系 准教授
学位
工学博士(東京大学)

J-GLOBAL ID
200901062630747582
researchmap会員ID
1000292029

論文

 81
  • 戸田 知朗
    電子情報通信学会 通信ソサイエティマガジン 17(4) 330 2024年  
  • Tatsuki Ikeuchi, Hiroyuki Sato, Yoshihisa Takayama, Tomoaki Toda
    Proceedings of 34th International Symposium on Space Technology and Science ISTS 2023-j-13 2023年6月  査読有り最終著者
  • Masato Tsuboi, Yutaka Hasegawa, Go Tabuchi, Yasuhiro Murata, Koji Yuchi, Tomoaki Toda, Takashi Uchimura, Kimihiro Kimura, Takashi Kasuga
    Publications of Astronomical Society of Japan 75(3) 567-583 2023年3月  査読有り
    We built a Ka-band dual-circular-polarization low-noise receiver for the Misasa 54 m parabola antenna in Misasa, Japan. The antenna is designed to be combined with a transmitter and receiver system at the X band (around 8 GHz) and simultaneously with a receiver system at the Ka band. The Ka band is the frequency band around 30 GHz, which is important for deep-space communications and radio astronomy. The receiver comprises some waveguide components including a feed horn, a circular polarizer, and low-noise amplifiers. The components are installed in a vacuum vessel and are cooled to 4 K with a Gifford-McMahon refrigerator, providing low-noise performance. The receiver is capable of simultaneously handling the left- and right-hand circular-polarization (LHCP and RHCP) channels. The receiver-noise temperature was measured to be T-RX similar or equal to 14 K in both the LHCP and RHCP channels. The system-noise temperature, including the antenna loss and atmospheric attenuation at the zenith, was measured to be T-sys = 36-37 K in both the LHCP and RHCP channels on a clear day in September at Misasa. When the receiver is used with the X-band transmitter, the system-noise temperature is maintained at T-sys similar or equal to 42 K in the RHCP channel. The degradation in the system-noise temperature is attributed to a frequency-selective reflector, which divides the signals in the X and Ka bands. There is no contamination from the transmitter to damage the receiver. The receiver has already been in use for deep-space communications and radio-astronomy observations. Our team in the radio-astronomy laboratory of ISAS/JAXA is responsible for the development of the receiver and the measurements of its performance.
  • Tomoaki Toda, Yuto Takei, Atsushi Fujii
    Hayabusa2 Asteroid Sample Return Mission 453-475 2022年  
  • K. Wada, K. Ishibashi, H. Kimura, M. Arakawa, H. Sawada, K. Ogawa, K. Shirai, R. Honda, Y. Iijima, T. Kadono, N. Sakatani, Y. Mimasu, T. Toda, Y. Shimaki, S. Nakazawa, H. Hayakawa, T. Saiki, Y. Takagi, H. Imamura, C. Okamoto, M. Hayakawa, N. Hirata, H. Yano
    Astronomy and Astrophysics 647 2021年3月1日  
    A projectile accelerated by the Hayabusa2 Small Carry-on Impactor successfully produced an artificial impact crater with a final apparent diameter of 14.5 ± 0.8 m on the surface of the near-Earth asteroid 162173 Ryugu on April 5, 2019. At the time of cratering, Deployable Camera 3 took clear time-lapse images of the ejecta curtain, an assemblage of ejected particles forming a curtain-like structure emerging from the crater. Focusing on the optical depth of the ejecta curtain and comparing it with a theoretical model, we infer the size of the ejecta particles. As a result, the typical size of the ejecta particles is estimated to be several centimeters to decimeters, although it slightly depends on the assumed size distribution. Since the ejecta particles are expected to come from a depth down to ∼1 m, our result suggests that the subsurface layer of Ryugu is composed of relatively small particles compared to the uppermost layer on which we observe many meter-sized boulders. Our result also suggests a deficit of particles of less than ∼1 mm in the subsurface layer. These findings will play a key role in revealing the formation and surface evolution process of Ryugu and other small Solar System bodies.

MISC

 102

担当経験のある科目(授業)

 1

所属学協会

 2

共同研究・競争的資金等の研究課題

 6

産業財産権

 2