• Tribology and Lubricants
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• 제14권4호
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• pp.114-120
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• 1998

The T-curve, wear and erosion behaviors of two different silicon carbides, i.e., the fine grained SiC and the in situ-toughened SiC(IST-SiC). Both materials exhibited an increasing T-curve behavior, although the T-curve of IST-SiC was steeper than that of fine grained SiC. The fracture toughness of IST-SiC was larger than that of fine grained SiC at long crack regime, whereas an opposite tendency occurred at short crack regime. The rate of material removal during wear and erosion tests was higher in IST-SiC compared to fine grained SiC. The difference between the material removal rates of two materials was discussed in the light of their R-curve behaviors.

• Journal of Astronomy and Space Sciences
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• 제18권1호
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• pp.55-62
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• 2001

W UMa 형 쌍성 TY UMa를 소백산천문대 61cm 반사망원경과 PM512 CCD 카메라를 이용하여 2001년 3월 19일부터 21일까지 3일간 측광관측하여 광도곡선을 완성하였다. 광도곡선의 형태는 제 2극심이 제 1극심보다 더 깊고, 식 바같부분의 max 1은 max II에 비하여 평균 $0.^m023$밝게 나타나는 비대칭이다. 비대칭 광도곡선을 분석하기 위하여 흑점 모델을 도입하고, Wilson & Devinney의 차등보정법을 이용하여 측광학적인 해를 구하였다.

• 천문학회보
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• 제42권2호
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• pp.63.3-64
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• 2017

KIC6118779 is an over-contact binary system having a short orbital period of about 0.36 days. The photometric data for this system are acquired by the observations of Kepler mission in the long cadence mode having a time resolution of about 30 minutes. It means that the Kepler light curves of the system may be strongly affected by phase smearing effect and the analysis of them without consideration of the phase smearing effect may result in wrong stellar properties. Additionally, this system also shows dynamical variation of light curve resulting from spot activity. For all those reasons, it is difficult to investigate KIC6118779, and the investigation should be carried out carefully. In this presentation, we introduce the phase smearing effect and carry out the light curve modeling with the 2015 version of the Wilson-Devinney binary code considering the phase smearing effect. Our results show that the system is a deep over contact binary system and has extremely low mass ratio of about 0.12. Moreover our spot modeling implies the cyclic migration of a big cool spot on the massive component.

• 천문학회보
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• 제44권2호
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• pp.64.3-64.3
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• 2019

A bright post-breakout emission was detected for a Type Ic supernova (SN Ic) LSQ14efd, which was among the first for SNe Ic. To explain the early-time light curve and color evolution, the effects of the circumstellar medium (CSM) are investigated. Four main parameters, CSM mass, CSM radius, nickel distribution, and explosion energy, are systematically explored in multi-group radiation hydrodynamics simulations, STELLA. Matching the model light curves and color evolution with the observation, we could constrain the parameter space and find out the best fit models. Our results imply that the progenitor suffered a strong mass loss shortly before the explosion and had a massive CSM of ~0.1 M_⊙.

• Journal of Astronomy and Space Sciences
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• 제7권1호
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• pp.57-69
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• 1990

The eighteen ultraviolet light curves of Epsilon Aurigae have been plotted using the integrated fluxes reduced from the 233 IUE low dispersion spectra taken between 1978 and 1986. The times of contacts and depth of eclipse have been determined from the light curves at the wavelength from 2550 $AA$ to 3050 $AA$. The UV light curves show two brightenings during the totality, the downward slope of the variation from the second to the third contacts, and asymmetry of the eclipse light curve. The two selected spectra note that the energy density distribution is not changed between the totality of the eclipse and out-of-eclipse.

• Journal of Astronomy and Space Sciences
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• 제14권1호
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• pp.59-66
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• 1997

V711 Tau의 채층활동을 조사하기 위하여 자외선 영역의 Mg II 방출선의 세기와 광도 변화의 상관 관계를 유추하였다. 첫째, 가시광선 영역의 광도곡선의 형태와 자외선 영역의 광도곡선의 형태를 비교하고, 둘째, IUE 고분산 스펙트럼에서 Mg II 방출선의 세기를 위상별로 측정하고 방출선 부근의 연속선을 이용하여 자외선 광도곡선을 완성하였다. 방출선의 세기와 광도곡선을 비교한 결과 방출선이 강하게 나타나는 위상, $0.^{p}4$에서는 광도가 어둡게 나타나 최소가 되고, 방출선의 세기가 약할 때는 광도가 밝아져서 최대가 되었다. 이는 자기장이 강한 위상에서는 채층활동과 흑점의 크기가 증가하고 반대로 자기장이 약한 위상에서는 채층활동과 흑점의 크기가 작다는 것을 뜻한다. 그러므로 자기장, 채층활동, 별 표면의 흑점과의 상관 관계가 밝혀지고, V711 Tau의 변광은 표면의 채층활동과 흑점에 의한 것이다.

• 천문학회보
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• 제44권1호
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• pp.48.2-48.2
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• 2019

Tidal disruption events (TDEs) provide evidence for quiescent supermassive black holes (SMBHs) in the centers of inactive galaxies. TDEs occur when a star on a parabolic orbit approaches close enough to a SMBH to be disrupted by the tidal force of the SMBH. The subsequent super-Eddington accretion of stellar debris falling back to the SMBH produces a characteristic flare lasting several months. It is theoretically expected that the bolometric light curve decays with time as proportional to $t^{-5/3}$. However, some of the observed X-ray light curves deviate from the $t^{-5/3}$ decay rate, while some of them are overall in good agreement with the $t^{-5/3}$ law. Therefore, it is required to construct the theoretical model for explaining these light curve variations consistently. In this paper, we revisit the mass fallback rates semi-analytically by taking account of the stellar internal structure, orbital eccentricity and penetration factor. We find that the mass fallback rate is shallower than the standard $t^{-5/3}$ decay rate independently of the polytropic index, and the orbital eccentricity only changes the magnitude of the mass fallback rate. Furthermore, the penetration factor significantly can modify the magnitude and variation of mass fallback rate. We confirm these results by performing the computational hydrodynamic simulations. We also discuss the relevance of our model by comparing these results with the observed light curves.

• 천문학회보
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• 제9권
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• pp.3.2-4
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• 1984

• 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.

• 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.