• 천문학논총
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• 제32권1호
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• pp.1-4
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• 2017

Some after-dinner thoughts on the giants of infrared space astronomy. I here describe important events in infrared astronomy starting from 1964 when I started working on my PhD. Here I describe how I became involved in IRAS, Infrared Space Observatrory (ISO), Herschel, Spitzer and AKARI, together with important events that led to these great missions.

• 한국초등과학교육학회지:초등과학교육
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• 제34권3호
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• pp.288-296
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• 2015

This study aimed to analysis of concepts and inquiry activities related to the 'Earth Science' area in the South Korean elementary school textbooks to the current and to seek the improvement of future textbook. For the study, we were collected South Korean elementary school textbooks to the current. After the collection had been made, we were analyzed related to the 'Earth' area in the South Korean elementary school textbooks and were extracted central concepts and inquiry activities. The result of this study: First, there were 'A change in the land', 'Strata and Fossil', 'Volcanoes and Earthquakes', 'Earth and Moon', 'The weather', 'The Solar system and the Star', and 'Seasonal Change' in the central concepts related to the 'Earth' area in the South Korean elementary school textbooks to the current. Second, central concepts were almost the same but the curriculum was changed. Third, inquiry activities also were confirmed to be maintained with little change. This result was believed that it can provide a variety of suggestions at this point in changing the curriculum.

• 한국지구과학회지
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• 제30권1호
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• pp.96-110
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• 2009

8학년(중학교 2학년)을 대상으로 '지구와 별' 단원의 지구계 수업 모듈을 개발하였다. 그리고 이 수업 모듈 중 태양계 행성을 학습하는 행성 리모델링 활동을 개발하였다. 이 활동의 핵심은 행성에 생명체가 살 수 있도록 행성을 리모델링하는 것이다. 본 연구에서는 쓰기와 그리기로 표현된 학생들의 생각의 시각화와 이를 통해 학생들의 이해를 해석하였다 학생들의 인지구조를 분석하기 위하여 4개로 법주화된 분석틀을 개발하여 적용하였다. 그리고 인지적 내용 특성을 분석하기 위하여 지구계의 구성 요소별 그리고 과학과 기술의 이용별로 분석 요소를 세분화하여 적용하였다. 행성 리모델링 활동을 통해 분석한 학생들의 인지에는 지구 소양과 같은 지구계 수업의 영향이 나타났다.

• 한국지구과학회지
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• 제30권5호
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• pp.611-621
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• 2009

Using the spectroscopic data secured with the Hamilton Echelle Spectrograph at Lick Observatory, we found the physical condition of the planetary Nebula NGC 6210. The spectral line profiles of the permitted and forbidden lines have been analyzed using IRAF and StarLink/Dipso. The hydrogen number densities ($N_H$) are 2,000-20,000 $cm^{-3}$, and the electron temperatures are 8,100-10,300 K based on the forbidden lines. The expansion velocities, derived from the Full Width at Half Maximum (FWHM) and the double peak of the line profiles, are in the range of 10 to $45\;kms^{-1}$. The expansion velocities imply a shell structure with an accelerated nebular gas. We also derived abundances from the permitted lines of CII, CIII, NII, NIII, OII, and OIII, which may have been formed through the fluorescence mechanism. NGC 6210 is likely to be evolved from a progenitor of more than $3M_{\bullet}$, which had been born near the Galactic plane.

• 한국지구과학회지
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• 제31권2호
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• pp.164-171
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• 2010

본 연구의 목적은 중학교 2학년 과학 '지구와 별' 단원의 학습에 3D 천문 프로그램(Starry Night pro 6.0)을 활용한 수업을 실시한 후 과학 학업성취도, 과학 관련 태도, 자기 주도적 학습능력에 미치는 영향을 분석하여 학습효과와 학생의 인식을 알아보는데 있다. 연구대상은 중학교 2학년 198명의 학생이며 6차시에 걸쳐 3D 천문 프로그램(Starry Night pro 6.0)을 활용한 수업을 실시한 후 적용하기 전과 후의 조사를 통하여 그 학습효과를 분석하였다. 검사결과는 독립표본 t-검정과 대응표본 t-검정을 이용하여 분석하였다. 첫째, 3D 천문 프로그램을 활용한 수업이 전통적 수업 보다 학업성취도에서 유의미한 효과가 있는 것으로 나타났다(p<.05). 그러나 3D 천문 프로그램을 활용한 수업이 과학 관련태도에 미치는 효과의 분석에서는 유의미한 효과가 없는 것으로 나타났으며(p>.05), 자기주도적 학습능력의 향상에는 효과적이라는 결과를 얻을 수 있었다(p<.05). 본 연구의 결과는 '3D planetarium software를 활용한 수업은 8학년 과학수업에서 효과적이었다는 것을 보여준다.'라고 끝마치고 있다.

• 대한지구과학교육학회지
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• 제11권2호
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• pp.107-115
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• 2018

지구의 모양을 아는 것은 지구과학 교육에서 중요한 성취기준이다. 이 연구의 목적은 학교 급별로 효과적인 지구의 모양 실험을 조사하여 학교 탐구실험에 도움을 주고자하는데 있다. 이를 위해 연구자는 지구의 모양을 학습하기 위한 다양한 실험 방법을 제시하고, 예비교사 26명에게 초등학교, 중 고등학교, 대학교 학생들에게 적절한 실험이 무엇인지 조사하였다. 그 결과 효과적인 지구의 모양 실험에 있어서 학교 급별로 차이가 있었다. 예비교사는 초등학생들에게는 '항구로 돌아오는 배의 돛 관찰하기 실험이 효과적일 것으로 생각하고 있었다. 그리고 중 고등학교 학생들에게는 지구의 위도에 따른 북극성 고도 비교하기 실험, 대학교 학생들에게는 지면의 높이에 따른 시야의 차이 비교하기 실험이 효과적일 것이라고 응답하였다. 예비교사는 학교 급별 효과적인 지구의 모양 실험을 선택할 때에는 실험 방법의 난이도, 추상적인 사고와 배경지식의 깊이 등이 고려되어야 한다고 생각하였다.

• 천문학회보
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• 제36권2호
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• pp.115.1-115.1
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• 2011

We analyzed the line profiles of the planetary nebula (PN) NGC 7009 secured with the Keck I HIES and BOES's spectral data. The 5 positions were taken over the nebular image, 4 points on the bright rim plus 1 point at the central position. The covered spectral wavelength range was $3250{\AA}-8725{\AA}$ in these observations. We decomposed the lines of HI, HeI, HeII, CII, NIII, [ClIII], [NII], [OII], [OIII], [SII], [SIII], [ClIII], and [ArIII] using the IRAF and StarLink/Dipso. After correcting the Earth's movement and the PN's radial velocities, -48.6 & -48.9 km/s, respectively, for the Keck & BOES, we produced the line profiles in a velocity scale. The zero velocity at each line profile clearly indicates which part of the components is approaching or receding, giving a general information of the kinematical structure. Almost all of the low-to-medium excitation lines, such as [NII], [SII], [O III], and [ArIII], secured at the central position and four positions along the major & minor axes, showed 3 components, double peak + a wide wing component, suggesting the fast outflow structures are present. The overall geometry is a prolate shell which also has a fainter outer shell in the halo zone, but there appears to be some peculiar sub-structures inside the main shell. The high excitation He I, HeII, NIII lines which might be formed close to the inner boundary of the shell show unusual features, completely different from the other lines. The HeII and these high excitation lines may be indicative of a relative recent fast outflow from the central star and the permitted lines such as NIII might be affected by the innermost structure. We discuss a possible presence of a jet-like fast outflow structure in an out-flow axis different from the main axis of the spheroid shell.

• 천문학회지
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• 제1권1호
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• pp.37-50
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• 1968

By comparison and analysis of the optical data of the two galactic clusters of Pleiades and h and x Persei and the radio data of the HI gas clouds which are related with those two clusters, the relative motions of those gas clouds with retpect to the two clusters were obtained. The three theories on the acceleration of HI gas cloud surrounding a star cluster by Blaauw. Oort and Spitzer, and Kahn were examined with the above obtained kinetic data of the Pleiades and the h and x Penei clouds. And it was shown that Blaauw's theory is applicable to the h and x Persoi clouds but not to the Pleiades, that Dart and Spitzer's theory can explain the motions of both clouds, and that Kahn's theory needs more improvement to be a complete one.

• 천문학회보
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• 제43권1호
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• pp.58.1-58.1
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• 2018

The redshift range $1.4{\lesssim}z{\lesssim}2.5$ is often called the 'redshift desert' because of the difficulties in measuring spectroscopic redshifts due to the shifting of the major spectroscopic features into near-infrared wavelength (Steidel et al. 2004). One of the most efficient and fast way to select galaxies at this redshift range is the BzK technique designed by Daddi et al. (2004). Combining deep BVRz data from Deep Lens Survey with the wide-field (~4.08 deg2) K-band image, we select 1200 star-forming BzKs (sBzKs) and 120 passive BzKs (pBzKs) at K < 21.25. We discuss about the photometric redshifts, star formation rates, and stellar mass of the selected BzKs. Possible large scale structure at $1.4{\lesssim}z$ < 1.6 based on the spatial distribution of the BzKs is also introduced.

• 천문학회지
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• 제2권1호
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• pp.1-9
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• 1969

On the instantaneous tidal relaxation approximation, formulae are derived for the ellipticities and virial theorem of a slightly flattened homogeneous rotating cluster (the largest axis of the cluster is directed towards the Galactic center), in terms of the Galactic tidal force and the characteristic intrinsic plus orbital angular velocity. The expression for a purely tidally-determined ellipticity is identical to that for an incompressible fluid body of uniform density. Orbital motion generally contributes significantly to the shape of the cluster. The virial theorem is identical to that for an isolated cluster except that the gravitational potential energy is multiplied by (1-${\chi}$), where ${\chi}$ is a positive tidal correction term. To obtain the actual mass of a cluster, the virial theorem mass based on an isolated cluster should be multiplied by the factor 1/(1-${\chi}$). The formulae are applied to open star clusters, the globular cluster ${\omega}$ Centauri, and dwarf elliptical galaxies in the Local Group.