The International Astronomy Olympiad (IAO) was established by the Euro-Asian Astronomical Society in order to disseminate astronomical knowledge, promote international cooperation in astronomical education area and recognize the importance of astronomy in far-reaching field of science and human culture. The first IAO competition was held at the Special Astrophysical Observatory of the Russian Academy of Sciences located in the north Caucasus of Russia in 1996. Since then, it has been held every year. This paper describes the present status of the IAO main regulations regarding its operation and major results by year, related institutions, and organizations. We created a scientific inquiry framework to analyze past IAO problems in the recognitive aspect in order to measure levels of the scientific knowledges and the scientific thinking abilities. Through this analysis, we can understand the current status of the IAO, and examine the future direction of Korea Astronomy Olympiad. Also, we can make preparation for the IAO competition and the education of delegates.

본 연구는 예비 중등교사들을 대상으로 지구 내부에서의 방사성 동위원소에 대한 예비 중등교사의 대안개념의 구조를 이해하는 것이다. 그들의 대안개념의 구조를 Lakatos의 방법론을 기준틀로 한 Niaz(1998)의 제안을 사용하여 분석하였다. 이 연구는 사범대학 과학교육과 3∼4학년 17명을 대상으로 하였다. 연구 방법으로는 개방형 질문지법(open-ended written questionnaire)을 사용하였다. 연구 결과, 예비 중등교사들은 지구내부에서 방사성 동위원소의 붕괴의 설명은 지층의 높은 열과 압력이 그들의 대안개념에 가장 큰 영향을 주고 있었다. 또한 우리가 제안한 과학개념구성을 위한 과학 철학적 수업전략에 따른 그들의 개념변화를 조사하였다.

이 연구는 예비 중등 교사들을 대상으로 Lakatos의 방법론에 따라서 "계절 변화의 설명"에 대한 대안 모형을 조사하였다. 조사대상은 사범대학 과학교육학부 74명이다. 조사 결과 계절 변화에 대한 예비 중등 교사들의 설명은 과학적 모형과 불일치하는 대안 모형들을 가지고 있었다. 이러한 명백한 불일치의 대안 개념은 어떤 일관성 있는 방향으로, 자신들이 가지고 있는 대안 모형의 핵심 신념을 사용한다고 가정함으로서 설명되어 진다고 우리는 주장한다. 따라서 이 연구에서는 예비 교사들의 대안 모형을 극복하기 위해서 먼저 그들이 가지고 있다고 가정할 수 있는 핵심 신념들과 가능한 근원들을 알아보는 것이다. 그러한 근원들 중에서 교과서가 예비 교사의 대안 모형의 근원을 제공할 가능성을 배제할 수는 없다.

The problem of the collapse of a self gravitating disk is here considered. We show self-similar solutions for the above problem under a modified viscous parameter. Surface density depends on rm in the inner region, where m is -1.6. Therefore growing central mass goes on without mass inflow to the system.

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.

A model for the distribution of stars in the disk and the spheroid of our Galaxy is reexamined from an edge-on view of the Galaxy obtained by selecting infrared sources from the IRAS Point Source Catalog. The sources are counted as a function of galactic latitude. longitude and 12μm 12μm apparent magnitude. The source counts are reasonably separated into the disk component and the spheroid component contributions and each of the contributions is further interpreted as a convolution of a spatial density distribution and a luminosity function based on the least-square fit method. The spatial density of the disk component has an exponential radial scale length of hR∼2.6kpc hR∼2.6kpc and the vertical distribution follows a canonical sech2 sech2 law with a scale height hz∼240pc hz∼240pc . The distribution of the spheroid component can be represented by an oblate spheriod with an axis ratio k∼0.61 k∼0.61 and a de Vaucouleurs' r1/4 r1/4 law with an effective radius of Re∼120pc Re∼120pc . The steep density gradient of the spheroid component is consistent with that of late M giants in the central bulge. The luminosity functions of the disk and the spheroid component stars resemble respectively those of the K luminosity function of disk M giants (Garwood and Jones 1986) and the bolometric luminosity function of M giants in bulge fields (Frogel et al, 1990).

원반 및 해일로의 이중역 (two-zone) 모형을 바탕으로하여 나선은하의 화학적 진화 모형을 만들었다. 모형의 검증을 위하여 구체적인 수치계산을 수행하고 그 결과를 태양 부근에서 관측된 중원소 분포 등, 화학적 진화와 관련된 제반 관측 사실과 비교함으로써 은하계의 진화를 추론하였다. 모형의 수치계산 결과에 의하면 나선은하의 화학적 진화는 헤일로외 붕괴 과정과 별탄생율에 크게 의존하며, 원반의 초기질량함수와 별탄생율에 따라 서로 다른 양상을 보인다. 태양 부근 원반의 중원소 분포 등을 성공적으로 설명할 수 있는 진화 모형에서, 별탄생율은 가스의 질량 또는 표면밀도의 멱승에 비례하거나 시간에 따라 단조 감소하는 지수함수로써 표현되며, 초기질량함수는 헤일로에서는 다양한 형태의 함수 모두로써 가능하지만, 원반의 경우에는 시간에 따라 변화하는 질량함수를 채택하여야 한다. 우리 은하의 헤일로의 고속붕괴 모형에서는 시간에 따라 지수함수로 변화하는 별탄생율이 관측과 부하되지만, 반면 저속붕괴의 경우에는 가스 질량의 멱함수로 표현되는 별탄생율이 관측과 부합된다.

A model for the galactic distribution of stars is developed by fitting IRAS 12㎛ source counts to the two-component density distribution of an exponential disk and an R~ spheroid. The model can reproduce the IRAS source counts fairly well when we assume the late type M giants mainly contribute to the 12 ㎛ luminosity function. By fitting the source counts we find he scale length and the scale height of the exponential disk are 2.2kpc and 300pc respectively. The axial ratio of the de Vaucouleurs spheroid is suggested to be 0.85, and the local spheroid to disk population ratio is found to be 1/300.

A scheme for installing the digital printing devices as an additional output system of photoelectric photometry is discussed. The digital printing devices consist of counter/integrator and printer interfaces for the digital printer HP 5055A. The integration gate time could be adjusted from 1 second to 99 seconds.