구름의 생성 원인은 상승기류에 의한 단열 냉각인데 이에는 대류에 의한 상승기류와 전선에 동반되는 상승기류가 있고 또 복사냉각과 한냉공기와 온난공기의 혼합 등이 있다. 이러한 구름의 생성원인에 따라 대기 중에 떠 있는 구름은 고도와 모양이 다양하다. 구름모양은 L. Howard가 1803년에 제창한 것에 기초를 두고 분류되어 있으며, 분류의 기본은 가늘고 긴 섬유모양의 구름, 층모양의 구름, 뭉게뭉게 쌓인 구름의 3가지 형태로 크게 구분되고, 고도와 형태에 따라 다시 10 류(類)로 세분되어진다. 대부분이 유형은 구름의 외관상 특징이나 대류의 강도와 같은 구조상의 차이에 따라 종(種)별로 더욱더 세분된다. 때로는 구름은 어떤 모양의 모체의 그 일부가 전혀 별개의 유형으로 발생하거나 모체 전체가 별개의 유형으로 변화하는데 이 경우에는 원래 유형의 구름을 어미 구름이라고 한다. 우리나라에서는 층적운, 고층운, 권운의 구름들이 자주 나타난다. 일반적으로 고층운, 층운, 층적운과 같은 층운형에서 비나 눈이 내리고, 적운형인 고적운, 적운, 적란운에서는 소나기, 우박이 내리거나 모체 전체가 별개의 유형으로 변화하는데 이 경우에는 원래 유형의 구름을 어미 구름이라고 한다. 우리나라에서는 층적운, 고층운, 권운의 구름들이 자주 나타난다. 일반적으로 고층운, 층운, 층적운과 같은 층운형에서 비나 눈이 내리고, 적운형인 고적운, 적운, 적란운에서는 소나기, 우박의 강수현상이 있다.

The climatological characteristics at the Choejung-san site were statistically analyzed using monthly normals for the various meteorological elements at Taegu meteorological station for 30 years from January 1960 to December 1990. Various synoptic weather conditions were classified by the estimated geostrophic wind speeds and direction determined using the 850 hPa geopotential height field for 10 years from December 1980 to November 1989. Also the analysis of number of clear days were monthly and seasonally performed using the satellite infrared image data which were obtained from GMS 5 for 5 years from December 1990 to November 1995. The results reveal that the meteorological environments of astronomical observation at Choejung-san site were very good conditions during three hours after midnight except for summer season.

We have investigated the astronomical observational environments at the Choejung-san GEODSS site which is located at the south of Taegu, Korea. As a part of the investigation, seeing and night sky brightness were measured outside nearby the GEODSS site using the Celestron 8-inch portable reflector with $192{\times}165$ pixels Lynxx CCD camera during the period of December 1994 to April 1996. The average seeing values of 4.8 arcsecond in B filter and 5.1 arcsecond in V filter were determined using the IRAF software. These values might be overestimated and would be reduced by at least 1 arc second in both filters if they were measured by more stable telescope system with solid mount and under a dome. We also compare the average seeing value at the GEODSS site with those at three other observatories, the Bohyunsan Optical Astronomy Observatory, the Sobaeksan Optical Astronomy Observatory, and the Seoul National University Observatory, for justification of the above guess. Unfortunately the night sky brightness measurement was not successful mainly due to the short exposure time. The utilizing plan of the GEOSS site is discussed based on the average seeing value, naked-eye sky brightness measurement, analysis of the existing thirty-year weather data and twenty-year urban planning of the metropolitan Taegu city for the year of 2016.

In order to discover the candidates of emission-line galaxies towards Hydra Void, objective-prism observations using U.K. Schmidt Telescope were carried out. To search the emission feature of [0III]λλ4959,5007 λλ4959,5007 for all objects on the plate, all observed prism plates were scanned with APM at the Royal Observatory and the copied direct R plates were scanned with PDS Microdensitometer operating in the Inter- University Center for National Science Research Facilities. By utilizing the "XIMTOOL" package, both spectral and direct images for the same field were displayed simultaneously on up and down windows separately. In case of distinct emission features for a certain object, corresponding direct object on the other window was examined through eyeballing to see whether this object is a galaxy. Through this procedure, we discovered in total 33 candidates of emission-line galaxies in a single field.

We have built a near-infrared imaging camera with a PtSi array detector manufactured by the Mitsubishi Company. The PtSi detector is sensitive in the wavelength range 1 to 5μm 5μm . Quantum efficiency of PtSi is much lower than that of InSb and HgCdTe types. However, the PtSi array has advantages over the latter ones: (i)The read-out noise is very low; (ii)the characteristics of the array elements arc uniform and stable; (iii)it is not difficult to make a large PtSi array; and (iv) consequently the price is affordably low. The array used consists of 512×512 512×512 pixels and its size is 10.2mm×13.3mm 10.2mm×13.3mm . The filter wheel of the camera is equipped with J, H, K filters, and an aluminum plate for measuring the dark noise. The dewar is cooled with liquid nitrogen. We have adopted a method of installing the clock pattern and the observing softwares in the RAM, which Gill he easily used for other systems. We have developed a software with a pull-down menu for operating the camera and data acquisition. The camera has been tested by observing δ δ Orionis.

We have developed a graphic software for image processing of astronomical data obtained by observational equipment in Astronomical Observatory of Kyung Hee University. The essential hardware for running our computer program is simply composed of a PC with the graphic card to handle 256 colors and the color graphic monitor, including CCD camera system. Our software has been programmed in WINDOWS to provide good environments for users, by using various techniques of image processing on astronomical image data recorded in FITS format by KHCCD program(Jin and Kim, 1994) with a compressional mode. We are convinced that our results will be a fundamental and useful technique in the construction of data processing system and can be effectively used in any other observatories, as well as in data processing system of Kyung Hee University.

We observed impact spots on Jupiter which were formed by the collision with fragments of Shoemaker-Levy 9 comet during the period from 17 July to 13 August, by using the SNU 61cm reflector combined with CCD camera and DBVRI filters. In order to get more clear image of impact spots, the observed data were processed by the unsharp masking method, high-pass filtering method and Richardson-Lucy algorithm after the basic processing through IRAF package. The sizes of impact spots range from 2000km to 1000km, and from this size, the original size of comet fragments before collision with Jupiter is estimated to be less than ∼3km ∼3km . From the observed rotating rate of impact spots, the rotational period of Jupiter is determined as 9h 9h 56m 56m 32s 32s at the southern latitude of 47∘∼49∘ 47∘∼49∘ .

We measured lagrangian currents in the coastal regions off east coast of Korea. The experiment sites are the Ulijin region where Polar Front of the East Sea is formed and the Ulgi region where coastal upwelling occurs frequently in summer. Each drifters are equipped with GPS receiver, and their trajectories are montiored by receiving the data transmitted from drifters through radio signal. The experiment with 'transmitting' GPS is very useful in monitering flows in coastal regions. Trajectories of drifters in the Uljin Polar Front region in October 1994 showed counterclockwise flow pattern. The flow pattern agrees with the SST distributions obtained from NOAA-11 AVHRR image for the same period. The lagrangian trajectories of drifters at 5m and 15m depths in the Ulgi region for normal period of April 1995 showed that the currents at the top 15m layer are almost uniform and their magnitude is 29cm/s. However, the currents, measured by KORDI, during the upwelling period of June 1994 showed that the currents at 5m depth were 1.2 times stronger than those at 15m depth. The current pattern in the Ulgi upwelling region agrees with the horizontal and vertical distributions of seawater temperature measured by NFRDA at the same period.

해상에서 어군의 행동과 분포상태를 탐지하여 그 정보를 원격으로 전송하기 위한 원격어군탐지기를 시험제작하고, 이들을 이용하여 서해의 고군산군도 연안에서 1994년 8월 8일, 18일~19일 및 9월 8~9일에 낭장망에 입망하는 어군의 유영층과 그 어획변동 등을 조사하고, 원격어군탐지기의 실용성을 평가하여 분석, 고찰한 결과는 다음과 같다. 1. 어획어종은 12종이었으며, 멸치(Engraulis japonica), 꼴뚜기(Loligo beka), 밴댕이(Harengula zunasi) 등이 전 어획량의 95%이상을 차지하였다. 2. 해상이 동국에서 탐지한 어군탐지기의 기록과 그것을 원격으로 전송한 선상고정국의 어군기록은 매우 잘 일치하였다. 3. 멸치는 유속이 0.6kt 이하로서 유속변화가 적은 경우에 어획이 많았으며, 유속이 0.6kt이상인 때에는 적어지는 경향을 나타내었다. 4. 어군의 유영층은 유속이 1kt이하에서 얕아지는 경향이 있었으며, 유속이 1kt이상이고 유속변화가 커지면 유영층에 큰 변동이 없으며, 이때 평균깊이는 약 4m였다. 5. 1회 조업당 어획량은 10~30 kg이었으며, 유향과 어구의 부설방향이 일치하지 않거나 유속이 너무 강해지면 어획이 적음을 알 수 있었다. 이상의 결과와 같이 본 연구에서 시험제작한 원격어군탐지기는 낭장망어업에서 어군의 행동과 분포에 관한 어업정보를 파악하는데 유효하게 사용할 수 있음이 확인되었다.