The Korea Astronomy and Space Science Institute (KASI) has been developing a next-generation coronagraph (NGC) in cooperation with NASA to measure the coronal electron density, temperature, and speed simultaneously, using four different optical filters around 400 nm. KASI organized an expedition to demonstrate the coronagraph measurement scheme and the instrumental technology during the 2017 total solar eclipse (TSE) across the USA. The observation site was in Jackson Hole, Wyoming, USA. We built an eclipse observation system, the Diagnostic Coronal Experiment (DICE), composed of two identical telescopes to improve the signal-to-noise ratio. The observation was conducted at four wavelengths and three linear polarization directions in the limited total eclipse time of about 140 seconds. We successfully obtained polarization data for the corona but we were not able to obtain information on the coronal electron temperature and speed due to the low signal-to-noise ratio of the optical system and strong emission from prominences located at the western limb. In this study, we report the development of DICE and the observation results from the eclipse expedition. TSE observation and analysis with our self-developed instrument showed that a coronagraph needs to be designed carefully to achieve its scientific purpose. We gained valuable experience for future follow-up NASA-KASI joint missions: the Balloon-borne Investigation of the Temperature and Speed of Electrons in the Corona (BITSE) and the COronal Diagnostic EXperiment (CODEX).

In a solar coronagraph, the most important component is an occulter to block the direct light from the disk of the sun. Because the intensity of the solar outer corona is 10−6 to 10−10 times of that of the solar disk (I⊙), it is necessary to minimize scattering at the optical elements and diffraction at the occulter. Using a Fourier optic simulation and a stray light test, we investigated the performance of a compact coronagraph that uses an external truncated-cone occulter without an internal occulter and Lyot stop. In the simulation, the diffracted light was minimized to the order of 7.6 × 10−10 I⊙ when the cone angle c was about 0.39◦. The performance of the cone occulter was then tested by experiment. The level of the diffracted light reached the order of 6 × 10−9 I⊙ at c = 0.40◦. This is sufficient to observe the outer corona without additional optical elements such as a Lyot stop or inner occulter. We also found the manufacturing tolerance of the cone angle to be 0.05◦, the lateral alignment tolerance was 45 μm, and the angular alignment tolerance was 0.043◦. Our results suggest that the physical size of coronagraphs can be shortened significantly by using a cone occulter.

목 적: 본 연구의 목적은 3D 안경 또는 스마트 글라스와 같은 대량생산형 안경테의 착용감을 평가하는데 있어 EEG 측정의 유용성을 보이는 것이었다. 방 법: 무작위 순서로 2 종류의 대량생산형 안경테(안경테-A와 -B)를 착용하고 있는 동안 40명의 피검자의 뇌파 강도를 주파수에 따라 측정하였다. 2 종류의 안경테에 대해서 측정된 α파의 시간에 대하여 평균 한 상대강도를 서로 비교하였다. 결 과: 안경테 A의 시간에 대하여 평균한 α파의 상대강도가 안경테 B의 시간에 대하여 평균한 α파의 상대강도보다 통계적으로 유의하게 더 강한 것으로 나타났다. 결 론: 시간에 대하여 평균한 α파의 상대강도는 대량생산형 안경테의 착용감을 상대적으로 비교하는데 있어 객관적인 지표로 활용될 수 있다.

The government expands its investment on R&D programs for economic growth, thus there are growing attention on the result of R&D programs. However, our existing research is in the circumstance of only measuring efficiency, but not reflecting unique characteristics of R&D programs. In this study, it provides more developed method for efficiency analysis in national R&D programs by using partial efficiency concept and measuring influence of input factors. It analyzes the influence of each input factor on efficiency by using partial efficiency concept. And it also determines input factors in similar influence throughout Spearman correlation coefficient. Finally, it suggests new method to improve discriminatory power of efficiency analysis by determining representative factors.

This study was decontaminant to use hydrogen peroxide(H2O2), surfactant and microbial and to use field contaminated soil experiment was to evaluate the adequacy and processing possibilities. A chemical oxidation was applied to using 5% concentration hydrogen peroxide more than 75% removal efficiency for TPH. Surfactant result of using SOR-100 1% 5,066 mg/kg to 796 mg/kg as the highest efficiency. Microbial injected 106 CFU/g soil in the soil by 45 days result of low-contaminated soil 1,325 mg/kg, removal rate was 57.7%.

The e-CALLISTO is a global network of frequency-agile solar radio spectrometers that was constructed in a collaboration between Swiss Federal Institute of Technology Zurich (ETH Zurich) and local host institutes. It is intended to monitor solar radio bursts 24 hours a day in frequency range between 45 MHz and 870 MHz. One of e-CALLISTO spectrometer was installed at Korea Astronomy and Space Science Institute (KASI) in 2007 October. The spectrometer gets signals from a horizontally polarized log-periodic antenna mounted on an automatic Sun-tracking system. Tracking status and data are monitored in Space Weather Monitoring Laboratory (SWML) of KASI in real time, and flare time data are transferred to ETH Zurich data archive daily. Using this spectrometer we obtained a couple of type II solar radio bursts on 2007 December 31, and found that these bursts are associated with a CME which occurred on the east limb.