We have investigated intensively an optical telescope with 76cm diameter and CCD camera system in astronomical observatory of Kyung Hee university, in order to maximize instrumental functions of our observational equipments and to construct a more reliable photometric system. And computer softwares AUTO DOME, KH CCD and KH PHO for astronomical image observations and their automatic photometries with high accuracy have been made for observers w use our observational system conveniently and efficiently. Throughout careful examinations of these programs, it has been proved that the observing time by our program is shorter than that by manual operations, so that, fast and accurate observations can be executed with ease. For open cluster NGC 7063 observed with S/N value of 350 or more by KH PHO, we have found the magnitude measurements of 11 object stars would show 0.007 magnitude difference, comparing with magnitude data from IRAF/APPHOT. From automatic photometry of eclipsing binary, AB And observed by our software, total 220 data points with good quality have been acquired during 8 hours and so we could make a better light curve than that obtained from any observational results by domestic photoelectric photometry system.

We observed the 2 mm ortho and para transitions of H213CO H213CO toward the Orion Molecular Cloud-1 using the 12 m NRAO telescope at Kitt Peak. Total column densities of 3×1014 3×1014 and 2.8×1012cm−2 2.8×1012cm−2 have been derived at KL and the approximately 3 are minute north from the KL (3N) position, respectively. We discuss the abundances, ortho/para ratios and its chemical implications.

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.

The small sized telescope can be best used if the control and observation can be made remotely and fully automatically by the aid of computers. We discuss the possible ways of automating the existing telescopes of various designs using personal computers. 'We have specifically designed the parts necessary to automate 16 inch Cassegrain Telescope at Pusan University Observatory. The degree of automation we have set for the present work is the interactive. remote observation including opening and shutting down of dome slit. The observational modes we have in mind are photoelectric photometry and CCD imaging. The basic components of the hardware are interface card for 16 or 32 bit IBM PC family of computers, relay switches for the control of telescope movements, stepping motor controller card for the control of observational equipments, and AID converter unit that accepts signal from sensors for the environment conditions such as temperature, wind speeds, precipitation, etc. We also have designed and built a photoelectric photometer that can be fully controlled by the command of a computer. Such observational equipment is also essential in order that the remote observation can be realized.

Wangjo Silok, the official chronicle of Lee Dynasty, carries 131 records on the Kepler Supernova 1604; all of them are given in the present report. Among them 112 records are detailed descriptions about the observed brightness variation over the period from October 13, 1604 (the 37th year of King Sunjo) to April 23, 1605. On July 14, 1605, an addendum is given as a final assessment of the guest star incidence. Since the apparent brightness, size and position are carefully described as compared to bright planets and stars, these records are ideal for retrieving light curve of the Kepler Supernova over the seven month period. Simple procedures are suggested for the derivation of light curve.

20cm 태양망원경이 소백산 천문대에서 대덕 천문우주과학연구소로 이전 설치된 후, 1987년 6월 19일 부터 1990년 11월 30일까지 흑점관측을 수행하여 343개의 흑점관측자료를 얻었다. 본 관측기간중 일일 평균 흑점상대수는 83.4로, 매일 평균 5개의 흑점군과 30개의 흑점이 관측되었다. 관측된 월평균 흑점상대수를 분석한 결과에 의하면 1986년 9월에 시작한 제22 태양활동 주기의 극대기는 1989년 9월경으로 밝혀졌다. 국제 흑점 상대수와 비교 가능한 292개의 관측 자료를 사용하여 대덕 태양망원경의 규격화 상수 K를 결정하였으며, 그 간은 소백산 천문대의 규격화 산수 0.87보다 큰 1.08로 밝혀진다.

최적제어이론은 -6유에서 무한대까지의 게인여유와 60˚의 위상여유, 그리고 원조건(Circle Condition)에 의해 보증되는 감도감소 등과 같은 로바스트성에 대한 긍정적인 면들을 가지고 있다. 이러한 결과는 전상태 피드백 경우일 때는 타당하지만, 실현문제에 있어, 관측기나 칼만필터가 사용되어질 경우에는 위의 조건이 완전히 만족하지 않는다. 본 논문에서는 관측기를 이용하여 다변수 제어계를 설계할 경우, 입「출력부분에서 안정여유가 회복될 수 있도록 하는 하나의 방법을 제안했다. 플랜트 입력과 출력에서 LQ가 보증하는 최소안정여유는 K=1의 경우에서도 회복될 수 있음을 보였다. 로바스트성 회복을 위해 본 논문에서는 종래의 방법(K=∞의 조건)과는 달리 유한값으로 하중행렬이 주어질 수 있으므로 본 방법은 하나의 명료한 로바스트성 회복법이라 할 수 있다. F=MC(or K=BM)를 만족하는 행렬 M이 존재하지 않을 경우, 그 해는 얻어질 수 없다. 그러나 K를 유한값으로 취했을 경우, 이 방법 이외의 또 다른 방법으로서는 입력과 출력에서 로바스트성 회복을 가지게 할 수 없을 것으로 생각된다.

달가림 관측을 목적으로 고속계수기를 설계, 제작하였다. 이 계수기는 외부 관측소로의 이동성, 비용의 절감, 제작의 편의성을 고려하여 애플 주변슬롯에 꽂히는 카드형식으로 설계되었으며, 운영을 위한 프로그램은 어셈블러로 작성되었다.