• 천문학회보
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• 제26권2호
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• pp.54.1-54.1
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• 2001

• 천문학회보
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• 제43권2호
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• pp.31.3-31.3
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• 2018

On August 17th 2017, for the first time in the history, the gravitational wave (GW) detectors recorded signals coming from the merger of two neutron stars. This event was named as GW170817, and more interestingly, gamma-ray emission was detected 2 seconds after the gravitational wave signal, and 11 hours later, telescopes in Chile identified that the GW signal came from the NGC 4993 galaxy at the distance of about 40 Mpc. This is again the first time that electromagnetic (EM) signals are detected for a GW source. The follow-up observations by astronomers all around the world, including our group in Korea, successfully identified the optical emission as the kilonova, the elusive optical/NIR counterpart that has been proposed to originate from a neutron star merger. This whole event started the new era of astronomy, so-called the "multi-messenger astronomy", where the combined information from GW and EM radiation reveals an unprecedented view of the universe. In this talk, I summarize this exciting event, and describe the efforts by Korean astronomers that have led to important discoveries about the kilonova and the host galaxy properties, and finally provide the future prospects.

• 한국초등과학교육학회지:초등과학교육
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• 제18권2호
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• pp.79-101
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• 1999

Astronomy is a good area to introduce a student to the study of science. The student often questions what causes the change in seasons, in the day and right, and in the rotation of stars, etc. Attempts to find answers to problems related to these astronomical observations influence the student`s intellectual development. This study is to investigate the effect of running an astronomical observations program on the preservice elementary teachers' astronomy achievement, astronomy teaching efficacy beliefs, and scientific attitude. Students consist of twenty four preservice elementary teachers. Three instruments are used: one is the astronomy achievement test, which is of an essay type, and 5 items. The other is the astronomy teaching efficacy beliefs test, which is of a Likert scale type, and 22 items. Another is the scientific attitude test, which is of the Likert scale type, and 10 items. Data are collected before and after instruction in the astronomical observations program, through the use of these tests. Data are compared. The results are: \circled1There is a significant difference between before and after instructions in the astronomy achievement test(t=11.31, p=000). \circled2There is a significant difference between before and after instructions in the astronomy teaching efficacy beliefs test(t=5.98, p=.000). \circled3There is a significant difference between before and after instructions in the scientific attitude test(t=270, pde. There fore, the a=.013). As a result, running an astronomical observations program has an effect on the preservice elementary teachers' astrono my achievement, astronomy teaching efficacy beliefs, and scientific attituuthor urges the teacher to teach astronomy through the astronomical observations in school.

• 천문학논총
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• 제20권1호
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• pp.97-107
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• 2005

We developed a data reduction program (RX) to process BOES data automatically. It processes a whole set of data taken during one night automatically - preprocessing, extraction to one-dimensional spectra and wavelength calibration. The execution is very fast and the performance looks pretty good. We described the performance of this program, comparing its procedure with that of IRAF. RX does not have functions for continuum normalization yet. We will develop those functions in the next works.

• 대한지구과학교육학회지
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• 제4권2호
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• pp.108-115
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• 2011

The purpose of this study was to develop and apply a creative problem-solving(CPS) program of instruction for earth science. After the earth science sections of high school science textbooks were analyzed, a theme of instruction was selected from the first-year unit 'the origin and evolution of the universe', and a CPS model of instruction. 32 high school sophomores and juniors who were the members of an astronomy club in the city of Gimhae, South Gyeongsang Province, participated in the program, and they took a test in scientific creative problem-solving skills before and after the experiment to grasp the effect of the program on their creative problem-solving skills. Besides, a survey was conducted to find out their awareness of the program. As a result of implementing the CPS program based on the CPS model of instructional for the unit 'the origin and evolution of the universe', the program turned out effective at boosting the scientific creative problem-solving skills of the students. To be specific, they made a significant progress in validity and scientificity, but that's not the case for elaboration and originality. When their awareness of the CPS program was checked, they expected the program to spark their interest in astronomy and be beneficial to the improvement of their creative problem-solving skills, but they didn't rate group activities high on the ground that the group activities weren't performed smoothly. The findings of the study suggest that the CPS instructional program for the unit 'the origin and evolution of the universe' based on the CPS model of instruction had a good effect on the improvement of the scientific creative problem-solving skills of the students.

• 천문학논총
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• 제21권2호
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• pp.101-112
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• 2006

We developed a new program for automatic continuum normalization of Echelle spectrographic data. Using this algorithm, we have determined spectral continuum of almost BOES data. The first advantage of this algorithm is that we can save much time for continuum determination and normalization. The second advantage is that the result of this algorithm is very reliable for almost spectral type of spectrum. But this algorithm cannot be applied directly to the spectrum which has very strong and broad emission lines, for example Wolf-Rayet type spectrum. We implanted this algorithm to the program which was developed in the previous study. And we introduced more upgraded BOES data reduction program. This program has more convenient graphical user interface environment, so users can easily reduce BOES data. Lastly, we presented the result of study on line profile variation of magnetic Ap/Bp stars analyzed using this program.

• 천문학회보
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• 제43권2호
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• pp.58.1-58.1
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• 2018

In the solar atmosphere, below the region of temperature minimum, temperature decreases with height and above it, temperature increases with height. Therefore the inference of temperature minimum is a basis of the study about the solar atmosphere and heating problem. The temperature of the temperature minimum region can be inferred from acoustic cutoff frequency. According to a recent study the acoustic cutoff frequency is related to the peak frequency of the power spectrum the chromospheric three-minute velocity oscillations. Using this relationship, we infer the temperature of temperature minimum. The three minute velocity oscillation and its power spectrum are obtained for a pore observed with the Fast Imaging Solar Spectrograph (FISS) $H{\alpha}$ band. We present the inferred temperature and compare it with the temperature of Maltby model. We also investigate the effect of the inclination of magnetic field on the temperature minimum.

• 천문학회보
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• 제25권2호
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• pp.50-50
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• 2000

• 대한지구과학교육학회지
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• 제13권1호
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• pp.100-109
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• 2020

이 연구의 목적은 과학문화 소외지역 초등학생들의 천문우주에 관한 동기유발과 천문우주 과학개념의 올바른 형성을 위해 STEAM 프로그램 및 PEST 방법을 적용한 '스타-카' 운영 프로그램을 개발하고, 이에 대한 효과를 살펴보는 것이다. 이를 위해 5명의 전문가가 참여하여 워크숍을 통해 프로그램 개발 방향을 설정하고, 이동천문대 프로그램 초안을 개발한 후, 1회의 시범 적용을 통해 프로그램을 최종 개발하였다. 이 연구에서 개발한 프로그램은 융합인재교육(STEAM)을 적용하였으며, 과학문화 소외지역 초등학생들을 대상으로 진행하는 프로그램이다. 연구 결과는 다음과 같다. 첫째, 이 연구에서 개발한 이동천문대 프로그램은 초등 전 연령이 함께 할 수 있는 천문우주에 대한 호기심을 자극하는 프로그램으로 개선하였다. 둘째, 이 연구에서 개발한 프로그램은 상황제시 1차시, 감성적 체험 5차시, 창의적 설계 5차시의 총 11차시로 구성하였다. 셋째, 이 프로그램에 참여한 학생들의 만족도 분석 결과는 대체적으로 효과가 있는 것으로 나타났다. 이러한 결과로 미루어볼 때, 이동천문대 프로그램은 학습자의 핵심 역량을 강화시킬 수 있을 것으로 기대된다.

• 천문학회지
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• 제52권1호
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• pp.11-21
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• 2019

Intensive Monitoring Survey of Nearby Galaxies (IMSNG) is a high cadence observation program monitoring nearby galaxies with high probabilities of hosting supernovae (SNe). IMSNG aims to constrain the SN explosion mechanism by inferring sizes of SN progenitor systems through the detection of the shock-heated emission that lasts less than a few days after the SN explosion. To catch the signal, IMSNG utilizes a network of 0.5-m to 1-m class telescopes around the world and monitors the images of 60 nearby galaxies at distances D < 50 Mpc to a cadence as short as a few hours. The target galaxies are bright in near-ultraviolet (NUV) with $M_{NUV}$ < -18.4 AB mag and have high probabilities of hosting SNe ($0.06SN\;yr^{-1}$ per galaxy). With this strategy, we expect to detect the early light curves of 3.4 SNe per year to a depth of R ~ 19.5 mag, enabling us to detect the shock-heated emission from a progenitor star with a radius as small as $0.1R_{\odot}$. The accumulated data will be also useful for studying faint features around the target galaxies and other science projects. So far, 18 SNe have occurred in our target fields (16 in IMSNG galaxies) over 5 years, confirming our SN rate estimate of $0.06SN\;yr^{-1}$ per galaxy.