예이츠의 희곡 『별나라에서 온 외뿔달린 백마』는 예이츠학자들이 실패 작으로 여기지만, 이 논문은 이 작품이 수작이라는 점을 증명하려한다. 먼저, 이 극의 대사를 보면, 인물들이 말을 많이 하는데 — 나오는 사람대부분이 그러한데 — 그렇지만, 그들의 말이 우아하고 열정이 넘친다. 즉, 일단의 거지들이 자신들의 생각을 마음껏 펼치는데, 모두, 거지가 아니라 시인처럼 말한다. 그들은 방언을 쓰지만, 애증이 섞인 감정들을 아름답고 생생하게 담고 있으며, 이 점이 이 극을 흥미롭고 의미 깊게 만든다. 두 번째 극의 구조로서 노래가 등장하는데, 예이츠의 노 드라마에서의 코러스의 역할을 한다. 이 논문은 극 중에서 중요한 시점마다 노래하는 것에 주목한다. 즉, 이 희곡은 결국 예이츠적인 극으로, 극 중에서 거지들이 거칠게 말하는 이상하게 매력적 인 토속어를 통해서 극이 아름답게, 세련되게 만든다. 또, 어떻게 정치적 문제들이 극의 중요 지점에서 시적으로 만들어지는지도 주목해야 한다. 한마디로, 이 극은 실패가 아니다. 아름답고 흥미로운 극으로 읽을 수 있다.

We map 6 massive young stellar objects (YSOs) in the CO J=2–1 line and survey 18 massive YSOs, including the six, in the HCO+ J=1−0, SiO J=2−1, H2O 616 − 523 maser, and CH3OH 70 − 61 A+ maser lines. We detect CO bipolar outflows in all the six mapped sources. Four of them are newly discovered (07299−1651, 21306+5540, 22308+5812, 23133+6050), while 05490+2658 is mapped in the CO J=2–1 line for the first time. The detected outflows are much more massive and energetic than outflows from low-mass YSOs with masses >20 M⊙ and momenta >300 M⊙ km s−1. They have mass outflow rates (3−6)×10−4 M⊙ yr−1, which are at least one order of magnitude greater than those observed in low-mass YSOs. We detect HCO+ and SiO line emission in 18 (100%) and 4 (22%) sources, respectively. The HCO+ spectra show high-velocity wings in 11 (61%) sources. We detect H2O maser emission in 13 (72%) sources and 44 GHz CH3OH maser emission in 8 (44%) sources. Of the detected sources, 5 H2O and 6 CH3OH maser sources are new discoveries. 20081+3122 shows high-velocity (>30 km s−1) H2O maser lines. We find good correlations of the bolometric luminosity of the central (proto)star with the mechanical force, mechanical luminosity, and mass outflow rate of molecular outflow in the bolometric luminosity range of 10−1−106 L⊙, and identified 3 intermediate- or high-mass counterparts of Class O objects.

As a part of the short-period variability survey (SPVS) at Bohyunsan Optical Astronomy Observa- tory, we obtained time-series BV CCD images in the region of the open cluster NGC 1039 (M34). The observations were performed for 22 nights from July 29, 2008 to September 26, 2010. We also made LOAO observations for 10 days from September 18, 2009 to October 30, 2010 to confirm the small variabilties of δ Scuti-type variable stars. In this paper we presented the observational properties of 28 variable stars found in the region. They are seven δ Scuti-type variable stars, two Doradus-type variable stars, four- teen eclipsing binary stars and five semi-long periodic or slow irregular variables, respectively. Only three variables were listed in the GCVS and the rest are newly discovered ones. We have performed multiple- frequency analysis to determine pulsation frequencies of the δ Scuti-type and ɤ Doradus-type variable stars, using the discrete Fourier transform and linear least-square fitting methods. We also have derived the periods and amplitudes of 12 eclipsing binaries from the phase fitting method, and presented the light curves of all variable stars.

이 연구의 목적은 중학교 천문 수업에 대한 과학 교사의 교수 실행에서 나타나는 시스템 사고를 분석하는 것이 다. 이를 위해 4명의 중학교 8학년 과학 교사의 천문 단원 수업을 녹화하였고 녹화된 수업은 모두 전사하였으며, 선행 연구의 시스템 사고 위계 구조를 수정하여 개발한 시스템 사고 분석틀을 적용하여 이들을 분석하였다. 또한, 수업 분석 후 참여 교사의 과학 수업에 대한 지향과 교수학적 생각을 심층적으로 분석하기 위해 비디오 자극 회상 면담을 실시하 였다. 연구 결과는 다음과 같다: 모든 참여 교사들은 천문 수업에서 시스템 사고의 위계를 제대로 반영하지 못하였으며, 낮은 수준의 시스템 사고만을 활용하는 것으로 나타났다. 또한, 교사가 학생 중심의 교수 지향을 지녔다 하더라도 시스 템 사고의 교수 실행은 교사 중심으로 진행되는 것으로 나타났다. 천문 수업의 교수 실행에서 시스템 사고가 부족하게 나타나는 것은 공간적 사고에 보다 집중하는 것과 지구과학 비전공 교사로서의 천문 내용 및 형성 평가 지식 부족 때 문인 것으로 판단된다. 이러한 연구 결과를 바탕으로 천문 수업에서 효과적인 시스템 사고의 도입 방안을 논의하였다.

Within the context of the hugely successful SAGE-LMC and SAGE-SMC surveys, Spitzer photometry observations of the Large and Small Magellanic Clouds have revealed millions of infrared point sources in each galaxy. The brightest infrared sources are generally dust producing and mass-losing evolved stars, and several tens of thousands of such stars have been classified. After photometrically classifying these objects, the dust production by several kinds of evolved stars - such as Asymptotic Giant Branch stars and Red Supergiants - can be determined. SAGE-Spec is the spectroscopic follow-up to the SAGE-LMC survey, and it has obtained Spitzer-IRS 5-40 μm spectroscopy of about 200 sources in the LMC. Combined with archival data from other programs, observations at a total of ~1000 pointings have been obtained in the LMC, while ~250 IRS pointings were observed in the SMC. Of these, a few hundred pointings represent dust producing and mass-losing evolved stars, covering a range in colors, luminosities, and thus mass-loss rates. Red Supergiants and O-rich and C-rich AGB stars - the main dust producers - are well represented in the spectroscopic sample. This paper will summarize what we know about the mineralogy of dust producing evolved stars, and discuss their relative importance in the total dust budget.

We review recent results on superhump period variations in SU UMa-type dwarf novae. Our statistical studies have revealed that the evolution of the superhump period is basically composed of three stages: stage-A, during which the superhump period is long and constant, stage-B, during which the superhump period increases as the superoutburst proceeds, and stage-C, during which the superhump period is short and constant. We also introduce a new method of estimating a mass ratio using the stage-A superhump period. This method can extend to, for example, low mass X-ray binaries or AM CVn stars if the stage-A superhump period is well determined.

We present the results of visual double stars speckle observations from 2013 using a Zeiss Double Refractor 60 cm with visual focal length f = 1,078 cm, and CCD SBIG ST-402 MEA. A Bessel V filter with ⋋ = 550 nm was placed in front of the CCD camera to reduce the chromatic aberration of the objective lens. The objects selected for this observation were calibration candidates and program stars with separations ranging from 0.9—6 arc second, and were located in both the northern and southern hemispheres. Seeing at Bosscha Observatory is generally 1—2 arc second, imposing a limit on visual double star separation below which the system cannot be resolved by long exposure imaging (longer than ~50 ms). Speckle interferometry methods are used to resolve double stars with separations below the typical size of seeing effects. A series of images were captured in fast short-time exposures (~50 ms) using a CCD camera. The result of our experiment shows that our system can be used to measure separations of 0.9 arc second (for systems with small Δm) and Δm ≈ 3.7 (for wide systems).

Close binary stars are so close that one component has an effect on the evolution of the other. But how do they form and evolve? This is an unsolved problem. One speculation is that the binary is a part of a hierarchical triple and its orbit shrinks due to interaction with the third component. Therefore, searching for and investigating tertiary components, especially close-in ones, in close binary stars are important for understanding their origin, as well as to test theories of star formation and stellar dynamical interaction.