• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2003년도 한국우주과학회보 제12권2호
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• pp.24-24
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• 2003

We present preliminary results about the quasi-simultaneous near-infrared light curves of the long-period eclipsing polar V1309 Ori in the J, H, K', and K bands with almost complete orbital phase coverage using the CFHT-IR camera. The optical light curve in the V and R bands, obtained by 1.8m Telescope at BOAO, will be also presented. The shape and the amplitude of the orbital light curve change significantly from optical to near-infrared wavelengths.

• Journal of Astronomy and Space Sciences
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• 제17권2호
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• pp.181-188
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• 2000

DO Cas는 최근 Shaw (1990)에 의해 근접촉쌍성으로 분류된 공전주기 0.68일의 식쌍성이다. 짧은 공전주기를 가짐에도 불구하고 Mannino (1958) 이후 분광관측에 의한 시선속도 곡선이 발표되지 않고 있다. 그런데 Hill (1991)은 Mannino의 시선속도곡선이 오류를 포함하고 있는 것으 로 보인다고 하였다. 이 연구에서 우리는 Asiago 천문대에 의뢰하여 Mannino가 분석한 분광관측 사진건판을 입수하여 PDS로 측정하여 IRAP로 재분석하였다. 이 시선속도곡선과 1998년에 관측한 BVR 광도곡선을 Wilson-Devinney 방법으로 동시에 분석하였다. 그 결과 DO Cas가 접촉 또는 주성이 로쉬엽을 채우고 있는 접촉에 매우 가까운 준분리형 쌍성임을 확인하였으며 또한 이 계의 절대량을 구하였다.

• Journal of Astronomy and Space Sciences
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• 제38권1호
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• pp.45-53
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• 2021

GLONASS, a satellite navigation system developed in Russia since 1976, is defunct and orbits in an unstable attitude. The satellites in these problems are not managed and there is no precise information, which can increase the risk of collisions with other space objects. In this study, detailed attitude dynamic have to be analyzed through photometry data, which requires spin period and spin axis. The light curve data is obtained by observing through the photometer at the Graz station and the power spectrum is calculated to obtain the cycle of the satellite. The geometric relationship between observer and sun is analyzed for GLONASS-50 satellite. The box-wing model is applied to obtain the phase reflection of the satellite and obtain the Irradiation of the satellite through this information. In Light Curve and Irradiation, the spin axis is calculated for each peak points with the distance square minimum technique. The spin axis of the GLONASS-50 satellite is RA = 116°, Dec = 92°.

• 천문학회보
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• 제43권2호
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• pp.59.1-59.1
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• 2018

SNe light curves have been used to understand the expansion history of the universe, and a lot of efforts have gone into understanding the overall shape of the radioactively powered light curve. However, we still have little direct observational evidence for the theorized SN progenitor systems. Recent studies suggest that the light curve of a supernova shortly after its explosion (< 1 day) contains valuable information about its progenitor system and can be used to set a limit on the progenitor size, R*. In order to catch the early light curve of SNe explosion and understand SNe progenitors, we are performing a ~8hr interval monitoring survey of nearby galaxies (d < 50 Mpc) with 1-m class telescopes around the world. Through this survey, we expect to catch the very early precursor emission as faint as R=21 mag (~0.1 Rsun for the progenitor). In this poster, we outline this project, and provide updates on IMSNG projects during 2017/2018 seasons.

• 대한수학회논문집
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• 제39권3호
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• pp.757-774
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• 2024

In three dimensional Euclidean space we consider kinematical invariants of the surface which is generated by the motion of a planar curve, especially, the surface which is foliated by circles. At first we characterize the properties of single parameter plane with the theories of unit spherical curve in three dimensional Euclidean space. Then using these results we give the invariants and differential invariants, kinematical properties and some special examples of the surface foliated by circles. The methods established here can be used to the other kinds of the surface in three dimensional Euclidean space.

• 호남수학학술지
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• 제43권1호
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• pp.88-99
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• 2021

The purpose of this paper is to assign a movable frame to an arbitrary point of a rational Bézier curve on the 2-sphere S2 in Euclidean 3-space R3 to provide a better understanding of the geometry of the curve. Especially, we obtain the formula of geodesic curvature for a quadratic rational Bézier curve that allows a curve to be characterized on the surface. Moreover, we give some important results and relations for the Darboux frame and geodesic curvature of a such curve. Then, in specific case, given characterizations for the quadratic rational Bézier curve are illustrated on a unit 2-sphere.

• 충청수학회지
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• 제24권4호
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• pp.665-673
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• 2011

In this paper, we derive a set of the partial differential equations that characterize an inelastic flow of a curve in a 3-dimensional Galilean space. Also, we give necessary and sufficient condition for an inelastic flow.

• Kyungpook Mathematical Journal
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• 제61권4호
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• pp.805-812
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• 2021

In this study, we obtain various conditions for the non-null curve flows to be inextensible in the 6-dimensional Lorentzian space 𝕃⁶. Then, we find partial differential equations which characterize the family of inextensible non-null curves.

• Journal of Astronomy and Space Sciences
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• 제23권4호
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• pp.311-318
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• 2006

ROTSE(Robotic Optical Transient Search Experiment) 후속관측을 통하여 W UMa형 식쌍성으로 재분류했던 변광성 중 광도곡선의 형태가 특이한 2개의 변광성에 대하여 2004년 5월 1일부터 5일간에 걸쳐 레몬산천문대 1m 망원경을 이용하여 고정밀 측광관측을 BVI 영역에서 수행하였다. W UMa형 식쌍성의 체계적인 분석을 위하여 2005년 개정한 Wilson-Devinney 쌍성코드를 사용하는 광도곡선분석 스크립트를 작성하였다. GSC2576-0319와 GSC2584-1731의 광도곡선을 분석하여 얻은 궤도경사각 (i)은 $43.^{\circ}5$와 $57.^{\circ}6$로써 비교적 낮은 값을 가지고 있으며, GSC2S84-1731의 광도곡선상 비대칭 효과를 설명하기 위하여 흑점모델을 적용하고, 이때의 흑점인자를 결정하였다.

• Journal of Astronomy and Space Sciences
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• 제13권1호
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• pp.19-31
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• 1996

We have analyzed collected photoelectric light curves for light variations of SW Lac. The method of Fourier analysis was adopted to quantify the light variation from season to season. We found the linear relation between the Fourier coefficient, B1 and the magnitude difference between two maxima. The total light of the system has been decreased as much as 0m.04 during approxiamately 20 years time interval. Photoelectric parameters including spot parameters for all light curves were obtained by the method of the Wilson and Devinney differential correction in order to secure the variations of parameters from season to season. SW Lac, not like RS CVn type stars, required to adjust all parameters as well as spot parameters for a reasonable fit to the observations of each epoch. A surface temperature of cooler star is one of the most sensitive parameters to affect a shape of light curve of SW Lac. We conclude that the shape of light curve of SW Lac varies even during one season as well as season to season. The light curve is mainly caused by inhomogeneous surface temperature due to strong chromospheric activity of the system.