zenichi yamamoto

GaN HEMT has been expected to satisfy requirements being used in space as amplifying devices of future high-efficiency onboard SSPAs due to its excellent properties such as robustness in a harsh environment, applicability to high frequency and high power operation. However, in X-band, the most important frequency band for space communication at this moment, evaluation of GaN HEMT to prove the space usage has not been conducted yet because ensuring a steady supply of X-band GaN HEMT devices is still difficult due to current collapse phenomena. Therefore, in this research, evaluation of RF characteristics affected by operational conditions and space environmental testing of X-band HPA using COTS GaN HEMT was conducted to secure the space usage.

High power operable and miniaturized rectifier is one of the most important issues for spacecraft health monitoring system. This is because the flexibility of location, number, and power consumption regarding sensor tag is indispensable for reliable health monitoring. Previous single rectifiers focusing on schottky diode are unsuitable since operating at high power and considering integrated MMIC sensor tags are quite difficult. This research proposes GaN HEMT based rectifier for these issues due to its excellent properties such as structurally-preferable for MMIC, and suitable for high power operation. Design and evaluation of GaN HEMT based rectifier and an experiment using the rectifier and a thermal sensor with microwave wireless power transfer has been conducted. The proposed rectifier can be operated with 47 dBm input RF signal.

The Radio Science experiment (RS) in the Akatsuki mission of JAXA aims to determine the vertical structure of the Venus atmosphere, thereby complementing the imaging observations by onboard instruments. The physical quantities to be retrieved are the vertical distributions of the atmospheric temperature, the electron density, the H2SO4 vapor density, and small-scale density fluctuations. The uniqueness of Akatsuki RS as compared to the previous radio occultation experiments at Venus is that low latitudes can be probed many times thanks to the near-equatorial orbit. Systematic sampling in the equatorial region provides an opportunity to observe the propagation of planetary-scale waves that might contribute to the maintenance of the super-rotation via eddy momentum transport. Covering the subsolar region is essential to the understanding of cloud dynamics. Frequent sampling in the subsolar electron density also helps the understanding of ionosphere dynamics. Another unique feature of Akatsuki RS is quasi-simultaneous observations with multi-band cameras dedicated to meteorological study; the locations probed by RS are observed by the cameras a short time before or after the occultations. An ultra-stable oscillator provides a stable reference frequency which is needed to generate the X-band downlink signal used for RS.

The electron density profiles above the lunar surface are being observed by the radio occultation technique during the mission using the Vstar and Rstar sub-satellites. In addition to a traditional technique which uses one orbiter, we are conducting another method which uses two orbiters with the second one being used to measure the terrestrial ionosphere contribution. Previous radio occultation measurements have indicated the existence of an ionosphere with densities of up to 1000 cm^-3 above the dayside lunar surface. These densities are difficult to explain theoretically when the removal of plasma by the solar wind is considered, and thus the generation mechanism of the lunar ionosphere is a major issue, with even the validity of previous observations still under debate. The SELENE radio science experiment will establish the morphology of the lunar ionosphere and will reveal its relationship with various conditions to provide possible clues to the mechanism.