• 천문학논총
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• 제30권2호
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• pp.715-718
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• 2015

Astronomy is a popular topic for the public in term of astronomical phenomenon such as occultations, solar and lunar eclipses or meteor showers. In term of education, astronomy also is popular as one of the world Science Olympiads. Social media, as the new trend in communicating and connecting people, plays a significant role in increasing the size of the astronomy community. Beyond IYA 2009, more and more astronomy activities have been done in many places in Indonesia. New astronomy communities have been formed in several cities and public engagement is also high in social media especially on Facebook and Twitter. In this paper, we will discuss the lesson learned from astronomy outreach achievements in Indonesia and the need for citizen science projects as a distance learning tool for the public as part of astronomy development in Indonesia. We argue and propose that this project will be also important up to a regional scope.

• 천문학논총
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• 제30권2호
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• pp.753-755
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• 2015

We had a campaign of observing the annular solar eclipse on 2012 May 21 by naked eye through eclipse eyeglasses to determine the limit line of annularity. As a result, we had about 15,000 reports through our website. In addition there were many observation groups for which about 30,000 people in total participated in the observations. The overall result was that the limit we observed by naked eye through eclipse glasses coincided with a prediction that took into account the lunar limb irregularity within the error of ${\pm}500m$. This error of the limit line location corresponds to about ${\pm}200km$ of the radius of the Sun.

• Journal of Astronomy and Space Sciences
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• 제8권2호
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• pp.149-158
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• 1991

Sixteen unitary Light curves of AR Lac in B and V are made at Yonsei University Observatory in the period of 1980-1988. Some overview findings of light variations are made. (1) The light variation outside eclipse follow none of the wave migration patterns reported by previous investigators. (2) Complicated shapes outside eclipse are apparently much reduced in the light curves of 1983-1984. This suggests than, in the future, AR Lac has a chance to attain a normal state with no complicated interactions. (3) The depths of the primary and the secondary mid-eclipses are changing year-to-year. (4) The K0 star, the larger component, has brightened by $0.^m$ 14 in V, while the G2 star has shown a fluctuation of about $0.^m$05 in V. (5) The B-V values at primary mid-eclipse have no correlation with the depth variations. (6) Independently of the increase of maximum brightness, the B-V colors in the non-eclipsed phases changed slightly over the years.

• 한국지구과학회지
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• 제29권4호
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• pp.352-362
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• 2008

본 연구에서는 통합교과적 접근이 필요한 지구과학 개념에 대한 예비 교사들의 이해를 알아보기 위하여 식 현상에 대한 예비 교사들의 정신 모형을 탐색하였다. 본 연구에는 30명의 중등 예비 지구과학 교사와 36명의 초등 예비교사들이 참여하였다. 정신 모형의 분석을 위해서 서로 다른 맥락의 질문지에 대한 예비 교사들의 응답 및 질문지를 토대로 한 심층 면담 과정에서 나타난 현상론적 초안과 전략적 국면을 분석하였다. 연구 결과, 식 현상에 대해 예비 교사들은 4개의 서로 다른 수준의 정신 모형을 가진 것으로 분석되었다: (1) 차폐 모형, (2) 공전궤도면 모형, (3) 혼성모형, 그리고 (4) 그림자 모형, 차폐 모형은 결함이 있는 모형이며, 공전궤도면 모형은 불완전한 모형, 그림자 모형은 과학적으로 옳은 모형이다. 혼성 모형은 두 개 이상의 정신 모형을 동시에 사용한다. 중등 예비 교사의 경우는 공전궤도면 모형이 40%로 가장 우세한 반면, 초등 예비 교사의 경우는 차폐 모형이 67%로 가장 많았다. 국면의 수준이 정신모형의 수준을 결정하며, 국면의 수준은 현상론적 초안에 의해 결정되는 것으로 분석되었다. 이 연구를 통해 정신 모형의 상황 의존성을 확인하였으며, 식 현상에 대한 낮은 수준의 정신 모형들이 개념적 모형으로 바뀌기 위해서는 광학과 기하학이 통합된 새로운 접근이 필요함을 알 수 있었다. 또한 정신 모형의 규명을 통한 예비 과학 교사의 주제 특정적 교과교육학 지식의 향상 가능성을 시사하였다.

• Journal of Astronomy and Space Sciences
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• 제31권3호
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• pp.187-197
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• 2014

We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to substellar nature, and were inferred from timing measurements of the system's primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behavior. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically viable explanation for measured eclipse timing variations. We conclude that dynamical considerations reveal that the proposed SW Lyncis multi-body system most likely does not exist or the companions have significantly different orbital properties from those conjectured in Kim et al. (2010).

• Journal of Astronomy and Space Sciences
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• 제6권2호
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• pp.127-135
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• 1989

연세대학교 천문대의 60cm와 40cm 반사망원경을 이용하여 1982년 4월 부터 1985년 5월까지 Epsilon Aurigae를 UBV 관전측광하여 총 1065 관측점을 얻었다. 우리의 광도곡선에 다른 천문대들의 관측자료를 합하여 제1극심의 광도곡선을 완성하였다. 이 광도곡선에서 2차적인 광도변화, 폭발현상, 식중심의 밝아짐 등에 관하여 자세히 조사하고, 제1그심의 각 접촉시각들과 중심식 시각을 결졍하여 다른 연국자들이 정한 값들과 비교하였다. 과거의 식들에서 구한 값들과 비교한 결과, 식이 일어나는 전체기간은 계속 감소하는 반면 완전식의 기간은 계속 증가하였다. 현재 가장 널리 통용되는 디스크 모델에 위의 여러 현상들을 적용하여 보았으나 명확히 설명되지 않았다. 그래서 새로운 모델인 혜성 모델을 만들어 광도곡선에 나타난 현상들을 해석하여 보았다.

• 천문학회보
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• 제37권2호
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• pp.109.1-109.1
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• 2012

In the past few years, two-planet circumbinary systems (e.g., HW Vir, NN Ser, DP Leo and HU Aqr) have been detected around short-period eclipsing binaries using ground-based telescopes. The existence of these planets has been inferred by interpreting the O-C variations of the mid-eclipse times. We have tested the orbital stability of these systems and propose to use Light Travel Time Effect (LITE) to detect such circumbinary planets from the ground. We generated synthetically the LITE signal of a two-planet circumbinary system with the aim to apply an analytic LITE model to recover the underlying synthetic system. To mimic a degree of realism inherent to ground-based observations, we added to the synthetic LITE data white noise with a Gaussian distribution and sampled the synthetic LITE signal randomly. We successfully recovered the original system demonstrating that two-planet circumbinary systems can be detected using ground-based telescopes, provided the timing measurements of the mid-eclipses are sufficiently accurate and the observing baseline is long enough to ensure a sufficient coverage of all involved periods. We used HU Aqr as a test system and applied our model to its proposed planetary bodies considering near-circular orbits. We present the results of our calculations and discuss the LITE-detectability of a HU Aqr-like system.

• Journal of Astronomy and Space Sciences
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• 제34권2호
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• pp.139-151
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• 2017

This paper presents an overview of deep space orbit determination software (DSODS), as well as validation and verification results on its event prediction capabilities. DSODS was developed in the MATLAB object-oriented programming environment to support the Korea Pathfinder Lunar Orbiter (KPLO) mission. DSODS has three major capabilities: celestial event prediction for spacecraft, orbit determination with deep space network (DSN) tracking data, and DSN tracking data simulation. To achieve its functionality requirements, DSODS consists of four modules: orbit propagation (OP), event prediction (EP), data simulation (DS), and orbit determination (OD) modules. This paper explains the highest-level data flows between modules in event prediction, orbit determination, and tracking data simulation processes. Furthermore, to address the event prediction capability of DSODS, this paper introduces OP and EP modules. The role of the OP module is to handle time and coordinate system conversions, to propagate spacecraft trajectories, and to handle the ephemerides of spacecraft and celestial bodies. Currently, the OP module utilizes the General Mission Analysis Tool (GMAT) as a third-party software component for high-fidelity deep space propagation, as well as time and coordinate system conversions. The role of the EP module is to predict celestial events, including eclipses, and ground station visibilities, and this paper presents the functionality requirements of the EP module. The validation and verification results show that, for most cases, event prediction errors were less than 10 millisec when compared with flight proven mission analysis tools such as GMAT and Systems Tool Kit (STK). Thus, we conclude that DSODS is capable of predicting events for the KPLO in real mission applications.

• 천문학회보
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• 제36권2호
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• pp.141.1-141.1
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• 2011

New CCD BVR light curves of BD And are presented. Our light curves with nearly equal depths for both primary and secondary eclipses show well-defined photometric waves outside eclipse for all of BVR bandpasses. The orbital period is greatly revised as $0.^d92580519$ which is twice longer than that known previously. Sixteen timings from our observations and thirteen ones from the SuperWASP measurements were calculated. All available timings over 76 years, including ours, were analyzed to figure out the dynamical behavior of the system. It was found that the recent CCD O-C residuals varied in a cyclical way with a period of $9.^y18$ and a semi-amplitude of $0.^d0046$. The secondary period of $9.^y18$ is the most shortest one among those which have been ever found in the short period RS CVn binary stars. The periodic variation most likely arises from the light-travel time effect due to a low-mass ($m_3{\sim}0.88\;M_{\odot}$) tertiary companion moving in an orbit with an large eccentricity ($e_3$=0.70) and a low inclination ($i_3{\sim}28^{\circ}$). The Applegate mechanism could not operate properly in both components because the model parameters require too much large luminosity changes of ${\Delta}L/L_{p,s}$ > 10. The new light curves were synthesized using the 2003 version of Wilson-Divinney code. It was found useful to model two huge spots on the surface of the hotter star and a third-light in order to minimize the residuals from the observations. Astronomical basic parameters were deduced from our photometric solution.

• 천문학논총
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• 제30권2호
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• pp.175-178
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• 2015

Due to the lack of an accretion disk in a polar (magnetic cataclysmic variable, MCV), the material transferred from the secondary is directly accreted onto the white dwarf, forming an accretion stream and a hot spot on the white-dwarf component. During the eclipses, different light components can be isolated. Therefore, the monitoring of eclipsing polars could provide valuable information on several modern astrophysical problems, e.g., CVs as planetary hosting stars, mass transfer and mass accretion in CVs, and the magnetic activity of the most rapidly rotating cool dwarfs. In the past five years, we have monitored about 10 eclipsing polars (e.g., DP Leo and HU Aqr) using several 2-m class telescopes and about 100 eclipse profiles were obtained. In this paper, we will introduce the progress of our research group at YNOs. The first direct evidence of variable mass transfer in a CV is obtained and we show that it is the dark-spot activity that causes the mass transfer in CVs. Magnetic activity cycles of the cool secondary were detected and we show that the variable mass transfer is not caused by magnetic activity cycles. These results will shed light on the structure and evolution of close binary stars (e.g., CVs and Algols).