Observations of the J=1-0 transition line of HCN were made at the center of Comet C/1995 O1 (Hale-Bopp) from November, 1996 to April, 1997 with the 14-m radio telescope at the TRAO (Taeduk Radio Astronomical Observatory). From the obtained data, an HCN production rate at each observed date was derived. The rapid variation of the HCN production rate near the perihelion was detected, and it is thought to be caused by jet(s) from the nucleus. The correlation between the visual magnitude and the HCN production rate is found to be QHCN=27.03−0.11(mv−5logΔ) QHCN=27.03−0.11(mv−5logΔ) .

We observed a total of 14 Mira variables as well as 4 late type variable stars for their SiO ν=1 ν=1 , J = 2 - 1 maser lines from April 1989 to November 1990 with the 13.7 m radio telescope at Daeduk Radio Astronomy Observatory. The maser intensity variations were the prime objective of the observations which well covered the periods of the variations. The origion of the variations were studied by comparing wi th those previousely measured in optical and infrared(IR) wavelengths and we confirmed that the intensity variations were in good correlation with those in V magnitude and IR intensity as previousely found in former investigators in general. However, for a few sources, we could find the missing maxima. The intensities themselves also were in good correlation with SiO ν=1 ν=1 , J = 1 - 0 maser intensities observed in Yebes as expected. The good correlations indicate that the pumping source of the SiO maser is likely to be the IR emission in the masing regions and the "missing maxima" that are apparent in two particular sources are considered to relate wi th the strength of shocks arising from the eruptive mass-loss from central stars.

We determined the efficiencies of the aperture. beam and forward spillover and scattering of 13.7 m radio telescope at Daeduk Radio Astronomy Observatory through the observations of the planets and Moon. The main panels adjustments were carried out on September 1991 and the improvements in the efficiencies were checked by comparing the observations made before and after the panel adjustments. The efficiencies were turned out to be 0.35, 0,47 and 0.83 at 115.27 GHz for the aperture, beam and forward scattering and spillover. respectively. These marked nearly a factor of two upgrade of the efficiencies previously measured.

본 실험은 수도이삭줄기의 유관속 발육을 증진시켜 수량을 증가시킬 수 있는 방안을 모색하기위하여 1989-1990년에 국제벼연구소(IRRI)에서 인도형인 IR58과 인본형인 Unbong 7을 공시하여 실시하였다. 1. 주간의 절간위치별 유관속수는 상위로부터 제1절간(수수절간)은 제 2,3,4,5절간에 비해 현저하게 적었으며, 품종별로는 IR58이 Unbong 7보다 많이 발육되었다. 2. 수수절간의 유관속수 및 횡단면적은 주간이 1,2차 분얼경보다 많이 컸으며, 분얼의 발육순서에 따라 저하되는 경향이었고, IR58은 Unbong 7보다 대유관속의 수와 횡단면적이 많이 컸으나 소유관속은 적고 작았다. 3. 양분의 이동통로인 사부와 수분의 이동통로인 본부의 횡단면적도 분얼의 출현이 빠른 것이 늦은것보다 크게 발육되어 있어서 출현이 빠르게 분얼경이 양수분흡수 및 동화물질의 전류에 유리한 특성을 가지고 있는 것을 사료되었다. 4. 이삭당 수중 및 수량은 주간에서 가장 높았고, 1차분얼 2차분얼의 순서로 낮아지는 경향으로 분얼경의 출현순서와 밀접한 관련성을 가지고 있었다. 5. 수수절간의 대유관속수는 이삭형질인 1,2차 지경수와 유의한 정의 상관관계를 나타냈으며, 이는 대유관속이 지경수 및 영화수 분화에 직접적인 영향을 준 것으로 해석되었다. 6. 일찍 출현된 분얼경은 늦게 출현된 분얼경에 비해 비교적 긴 생육기간을 가지고 있었으며, 양호한 유관속의 발육, 굵은 수수직경, 영화수 분화 및 등숙율을 향상시키고 나아가서 수량이 많아지는 특성을 나타냈다.