2017년 한해 동안 9개 공항만에서 중국 등 32개국, 120개 품목 8,660건을 조사한 결과, 523건에서 해충 검출이 있었다. 반입빈도가 높은 품목은 사과, 망고, 감귤, 배, 복숭아, 바나나, 오렌지, 오이, 고추. 호두(미탈각), 자두, 드래곤프릇, 포멜로, 토마토, 풋콩, 망고스틴, 대추 등의 순이었으며, 중국, 베트남, 일본, 필리핀, 대만, 태국 등의 나라에서 반입건수가 많았다. 해충 검출 빈도가 높은 품목은 망고스틴, 망고, 사과, 슈가애플, 람부탄, 고추, 자두, 구아바 등이며, 해충 검출 빈도가 높은 국가는 중국, 베트남, 태국 등이었다. 검출 해충류 중 금지해충으로 오리엔탈과실파리류(Bactrocera dorsalis sp. complex) 52건, 오이과실파리(Bactrocera cucurbitae) 1건, Bactrocera latifrons 2건이 있었으며, 과실파리류 32건이 동정중이며, 코드린나방(Cydia pomonella)이 1건 검출되었다.

The beam size and the antenna efficiency of TRAO 14m radio telescope were measured at 86.2, 98.0 and 115.2 GHz. The beam size was determined by deconvolving the azimuthal scanning data of the Venus. To test the accuracy of our deconvolution method, the beam size at 86.2 GHz was compared with that determined from the mapping data of SiO maser line and we found no difference between them. With above beam sizes, antenna efficiencies were calculated from the continuum measurements of Venus, Jupiter and Moon. The beam efficiencies at these frequencies are appeared to be 0.49, 0.45 and 0.41, respectively. On the other hand, we also suggest that an automatic focus setting can be adopted for TRAO radio telescope based on the gradual change of best focus with elevation.

We have studied the IR properties of molecular clouds in the region of the supershell GS234-02 using IRAS and COBE data. The mean values of dust color temperature and optical depth at 240μm are derived to be 15.4±1.5 K and 9.0±5.7×10-4, respectively, which agree well with those determined by Sodroski et al.(1994) for the outer Galaxy. Mean IRAS colors, R12/100= 0.074, R25/100= 0.052, R60/100= 0.219, indicate that the abundance of PAHs is enhanced but other particles are nearly the same as those of the solar neighborhood. We found the anticorrelation between R100/140 and R140/240. It cannot be explained by the thermal emission of traditional big grains. The anticorrelation implies that, at high ISRF, T100/140 underestimates the equilibrium temperature, while T140/240 overestimates it and, at low ISRF, vice versa. Therefore we propose to use the intensity ratio, R100/240 as a dust thermometer.

We present the data of photoelectric photometric observations of BW Vul carried out for four nights during the period of 1982 ∼ 1984 . The light curves with asymmetric shape show a stillstand on the ascending branch at phase of ϕ ≈ 0.85 just before the maximum light, and also the ampitude and shape of light curves are changed from night to night. Using all the published data, a new ephemeris of maximum time is derived, in which the period of light variation is P = 0 d .20102977 and its increasing rate is 2.2 see/century.

UBV photoelectric observations were carried out for bright stars in M67 and the masses of clump stars and giant stars were derived in M67 and the other old open clusters, NGC 188, NGC 2420, NGC 2506 and IC 4651. The mean mass of clump stars in the five clusters ranges m = 0.5 ∼ 1.0 m ⊙ , and its ratio to the mean mass of giant stars is about 0.83. The number ratio of blue stragglers to the stars brighter than the turn-off of main sequence increases with cluster age whereas that of clump stars decreases with age. These results imply that the clump stars and blue stragglers are at the phase of horizontal branch evolution.